List of exoplanet extremes#Planetary characteristics

The following are lists of extremes among the known exoplanets. The properties listed here are those for which values are known reliably. The study of exoplanets is one of the most dynamic emerging fields of science, thus these values may change as new discoveries are made.

Extremes from Earth's viewpoint

class="wikitable sticky-header"
Title ! Planet ! Star ! Data ! Notes
Most distant discovered \| SWEEPS-11 / SWEEPS-04 \| SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6 \| 27 700 light-years{{cite web \|title=Planetary Systems Composite Data \|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars \|website=NASA Exoplanet Archive \|access-date=12 December 2021}} \|Assuming the largest distance from the microlensing light-curve, the planet OGLE-2017-BLG-0364Lb might be more distant, at around 32 600 light-years (10 000 pc).{{Cite journal \|last1=Gui \|first1=Yuqian \|last2=Zang \|first2=Weicheng \|last3=Zhai \|first3=Ruocheng \|last4=Ryu \|first4=Yoon-Hyun \|last5=Udalski \|first5=Andrzej \|last6=Yang \|first6=Hongjing \|last7=Han \|first7=Cheongho \|last8=Mao \|first8=Shude \|last9=Authors) \|first9=(Leading \|last10=Albrow \|first10=Michael D. \|last11=Chung \|first11=Sun-Ju \|last12=Gould \|first12=Andrew \|last13=Hwang \|first13=Kyu-Ha \|last14=Jung \|first14=Youn Kil \|last15=Shin \|first15=In-Gu \|date=July 2024\|title=Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets \|journal=The Astronomical Journal \|language=en \|volume=168 \|issue=2 \|pages=49 \|doi=10.3847/1538-3881/ad4ce5 \|doi-access=free \|bibcode=2024AJ....168...49G \|issn=1538-3881}} PSR J0738-4042 at 37 000 ly was shown to be affected by a disk of asteroids but no planets have been detected yet.{{cite news \| url=http://www.science20.com/news_articles/rocks_around_clock_star_psr_j07384042_constantly_pummelled_asteroids-130121 \| title=Rocks Around The Clock: Star PSR J0738-4042 Is Constantly Pummelled By Asteroids \| work=Science 2.0 \| date=2014-02-20 \| accessdate=2014-02-23 }} The most distant potentially habitable planet confirmed is Kepler-1606b, at 2870 light-years distant,{{Cite web\|title=Exoplanet-catalog-Exoplanet exploration-Kepler-1606b\|date=10 May 2016 \|url=https://exoplanets.nasa.gov/exoplanet-catalog/2252/kepler-1606-b/}} although the unconfirmed planet KOI-5889.01 is over 5000 light-years distant. On 31 March 2022, K2-2016-BLG-0005Lb was reported to be the most distant exoplanet discovered by the Kepler telescope, at 17 000 light-years away.{{cite journal \|author=Specht, D. \|display-authors=etal\|title=Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing\|journal=Monthly Notices of the Royal Astronomical Society \|year=2023 \|volume=520 \|issue=4 \|pages=6350–6366 \|arxiv=2203.16959\|doi=10.1093/mnras/stad212 \|doi-access=free }} Among rogue planets, the furthest are very likely extragalactic planets within the lensing system SDSS J1004+4112 at 6.3 billion light-years.{{Cite journal \|last1=Bhatiani \|first1=Saloni \|last2=Dai \|first2=Xinyu \|last3=Guerras \|first3=Eduardo \|date=November 2019 \|title=Confirmation of Planet-mass Objects in Extragalactic Systems \|journal=The Astrophysical Journal \|language=en \|volume=885 \|issue=1 \|pages=77 \|arxiv=1909.11610 \|bibcode=2019ApJ...885...77B \|doi=10.3847/1538-4357/ab46ac \|issn=0004-637X \|doi-access=free}}
Least distant \| {{nowrap\|Proxima Centauri b}} \| {{nowrap\|Proxima Centauri}} \| 4.25 light-years \| Proxima Centauri b is the closest potentially habitable exoplanet known. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25 000 years), this is an absolute record.
Most distant directly visible \| CT Chamaeleontis b \| CT Chamaeleontis \| 622 light-years \| The resolved likely close to equal mass binary brown dwarf NIRISS-NGC1333-10 AB, the mass of NIRISS-NGC1333-10 B is slightly higher than the deuterium burning limit, is more distant at 978 light-years.{{Cite journal \|last1=Langeveld \|first1=Adam \|last2=Scholz \|first2=Aleks \|last3=Mužić \|first3=Koraljka \|last4=Jayawardhana \|first4=Ray \|last5=Capela \|first5=Daniel \|last6=Albert \|first6=Loïc \|last7=Doyon \|first7=René \|last8=Flagg \|first8=Laura \|last9=de Furio \|first9=Matthew \|last10=Johnstone \|first10=Doug \|last11=Lafrèniere \|first11=David \|last12=Meyer \|first12=Michael \|date=2024-08-22 \|title=The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-Floating Planets \|journal=AJ \|volume=168 \|issue=4 \|page=179 \|arxiv=2408.12639 \|doi=10.3847/1538-3881/ad6f0c \|doi-access=free}} The disputed planet CVSO 30 c may be more distant, at 1200 light-years away. The candidate planet AT Pyxidis b may also be more distant, at ~1207 light-years away.{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — AT Pyx b. \|url=https://exoplanet.eu/catalog/at_pyx_b--10507/}} Among rogue planets, o005 s41280 is the most distant at 17 300 light-years, followed by A2744-BD-1, at 15 520 light-years away.{{Cite journal \|arxiv=2501.16648 \|last1=Tu \|first1=Zhijun \|last2=Wang \|first2=Shu \|last3=Chen \|first3=Xiaodian \|last4=Liu \|first4=Jifeng \|title=Three Brown Dwarfs Masquerading as High-Redshift Galaxies in JWST Observations \|journal=The Astrophysical Journal \|date=2025 \|volume=980 \|issue=2 \|page=230 \|doi=10.3847/1538-4357/adaf9f \|doi-access=free \|bibcode=2025ApJ...980..230T }}{{Cite journal \|arxiv=2308.10900 \|last1=Langeroodi \|first1=Daniel \|last2=Hjorth \|first2=Jens \|title=Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei \|journal=The Astrophysical Journal \|date=November 2023 \|volume=957 \|issue=2 \|pages=L27 \|doi=10.3847/2041-8213/acfeec \|doi-access=free}} As free-floating objects, both of them might not be considered as planets, although their masses might be below 13 M_J.{{cite journal \|last1=Basri \|first1=Gibor \|last2=Brown \|first2=E. M. \|date=May 2006 \|title=Planetesimals to Brown Dwarfs: What is a Planet? \|journal=Annual Review of Earth and Planetary Sciences \|volume=34 \|pages=193–216 \|arxiv=astro-ph/0608417 \|bibcode=2006AREPS..34..193B \|doi=10.1146/annurev.earth.34.031405.125058 \|s2cid=119338327}}
Closest directly visible \|Epsilon Indi Ab \|Epsilon Indi \| 12.05 light-years \| {{nowrap\|COCONUTS-2b at 35.5 light-years is the}} next closest directly visible.
Star with the brightest apparent magnitude with a planet \| Alpha Arietis b \| Hamal{{Efn\|Algieba is mentioned to have a slightly higher magnitude (1.99); however it is the combined magnitude of the system and not of the planet-hosting star, which is 2.37.}} \| Apparent magnitude is 2.005 \| Alpha Centauri A (apparent magnitude 0.01) has a directly imaged candidate planet.{{cite journal \|last1=Wagner \|first1=K. \|last2=Boehle \|first2=A. \|last3=Pathak \|first3=P.\|last4=Kasper \|first4=M.\|last5=Arsenault\|first5=R. \|last6=Jakob\|first6=G.\|last7=Käufl\|first7=U. \|last8=Leveratto\|first8=S.\|last9=Maire\|first9=A.-L.\|last10=Pantin \|first10=E.\|last11=Siebenmorgen \|first11=R. \|last12=Zins\|first12=G. \|last13=Absil\|first13=O. \|last14=Ageorges \|first14=N. \|last15=Apai \|first15=D. \|last16=Carlotti\|first16=A. \|last17=Choquet\|first17=É.\|last18=Delacroix\|first18=C.\|last19=Dohlen\|first19=K.\|last20=Duhoux\|first20=P.\|last21=Forsberg\|first21=P.\|last22=Fuenteseca\|first22=E.\|last23=Gutruf\|first23=S.\|last24=Guyon\|first24=O.\|last25=Huby\|first25=E.\|last26=Kampf\|first26=D.\|last27=Karlsson\|first27=M.\|last28=Kervella\|first28=P.\|last29=Kirchbauer\|first29=J.-P.\|last30=Klupar\|first30=P. \|last31=Kolb\|first31=J.\|last32=Mawet\|first32=D.\|last33=N'Diaye\|first33=M.\|last34=Orban de Xivry\|first34=G.\|last35=Quanz\|first35=S. P.\|last36=Reutlinger\|first36=A.\|last37=Ruane\|first37=G.\|last38=Riquelme \|first38=M. \|last39=Soenke\|first39=C.\|last40=Sterzik\|first40=M.\|last41=Vigan\|first41=A.\|last42=de Zeeuw\|first42=T. \|display-authors=6 \|title=Imaging low-mass planets within the habitable zone of α Centauri \|journal=Nature Communications\|date=10 February 2021\|volume=12\|issue=1\|page=922\|doi=10.1038/s41467-021-21176-6\|pmid=33568657\|pmc=7876126\|doi-access=free\|arxiv=2102.05159\|bibcode=2021NatCo..12..922W}} [https://www.youtube.com/watch?v=Da2EMPuGu00&feature=youtu.be Kevin Wagner's (lead author of paper?) video of discovery] The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.{{cite press release \| title= NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega \| url=http://www.nasa.gov/home/hqnews/2013/jan/HQ_13-006_Vega_Asteroid_Belt.html \| publisher=Whitney Clavin, NASA \| date=8 January 2013 \| access-date=4 March 2013}} {{As of\|2021}}, a candidate planet around Vega has been detected.{{cite journal \|last1=Hurt \|first1=Spencer A. \|last2=Quinn \|first2=Samuel N. \|last3=Latham \|first3=David W. \|last4=Vanderburg \|first4=Andrew \|last5=Esquerdo \|first5=Gilbert A. \|last6=Calkins \|first6=Michael L. \|last7=Berlind \|first7=Perry \|last8=Angus \|first8=Ruth \|last9=Latham \|first9=Christian A. \|last10=Zhou \|first10=George \|title=A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets \|journal=The Astronomical Journal \|date=21 January 2021 \|volume=161 \|issue=4 \|page=157 \|doi=10.3847/1538-3881/abdec8 \|arxiv=2101.08801 \|bibcode=2021AJ....161..157H \|s2cid=231693198 \|doi-access=free }} Aldebaran (apparent magnitude varies between 0.75 and 0.95) was thought to have a candidate planet, however later studies found the existence of the planet inconclusive.{{cite journal \|last=Reichert \|first=Katja \|arxiv=1903.09157 \|title=Precise radial velocities of giant stars XII. Evidence against the proposed planet Aldebaran b \|journal=Astronomy & Astrophysics \|date=25 March 2019\|volume=A22 \|page=625 \|doi=10.1051/0004-6361/201834028 \|bibcode=2019A&A...625A..22R \|s2cid=85459692 }} Similarly, Pollux (apparent magnitude = 1.14) and Mirfak (apparent magnitude = 1.806) were claimed to have orbiting planets, both of which have been questioned.{{citation \|last1=Ducati \|first1=J. R. \|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system \|date=2002 \|journal=CDS/ADC Collection of Electronic Catalogues \|volume=2237 \|pages=0 \|postscript=. \|bibcode=2002yCat.2237....0D \|doi=10.26093/cds/vizier \|id=VizieR Cat. II/237/colors \|doi-access=free}}{{cite conference \|last1=Aurière \|first1=Michel \|last2=Konstantinova-Antova \|first2=Renada \|display-authors=etal \|date=August 2014 \|title=Pollux: a stable weak dipolar magnetic field but no planet? \|conference=Magnetic Fields throughout Stellar Evolution \|volume=302 \|pages=359–362 \|arxiv=1310.6907 \|bibcode=2014IAUS..302..359A \|doi=10.1017/S1743921314002476 \|book-title=Proceedings of the International Astronomical Union}}{{cite journal \|last1=Aurière \|first1=M. \|last2=Petit \|first2=P. \|display-authors=etal \|date=February 2021 \|title=Pollux: A weak dynamo-driven dipolar magnetic field and implications for its probable planet \|journal=Astronomy & Astrophysics \|volume=646 \|issue= \|pages=A130 \|arxiv=2101.02016 \|bibcode=2021A&A...646A.130A \|doi=10.1051/0004-6361/202039573}}{{cite journal \|bibcode=2012A&A...543A..37L \|title=Detection of the 128-day radial velocity variations in the supergiant α Persei. Rotational modulations, pulsations, or a planet? \|journal=Astronomy and Astrophysics \|volume=543 \|pages=A37 \|last1=Lee \|first1=B. -C \|last2=Han \|first2=I. \|last3=Park \|first3=M. -G. \|last4=Kim \|first4=K. -M. \|last5=Mkrtichian \|first5=D. E. \|year=2012 \|arxiv=1205.3840 \|doi=10.1051/0004-6361/201118539 \|s2cid=118482287 }} An Earth-mass planet claimed to orbit Alpha Centauri B (apparent magnitude = 1.33) was subsequently refuted.{{cite journal \|last1=Rajpaul \|first1=Vinesh \|arxiv=1510.05598 \|title=Ghost in the time series: no planet for Alpha Cen B \|date=19 October 2015 \|doi=10.1093/mnrasl/slv164 \|volume=456 \|journal=Monthly Notices of the Royal Astronomical Society: Letters \|issue=1 \|pages=L6–L10\|doi-access=free \|bibcode = 2016MNRAS.456L...6R }} A 2023 study detected 10 luminous point sources around the primary star of Fomalhaut system (apparent magnitude = 1.16), of which the last source may or may not be a planetary-mass companion.{{cite journal \|last1=Ygouf \|first1=Marie \|last2=Beichman \|first2=Charles \|display-authors=etal \|title=Searching for Planets Orbiting Fomalhaut with JWST/NIRCam \|journal=The Astronomical Journal \|date=October 2023 \|volume=167 \|issue=1 \|page=26 \|doi=10.3847/1538-3881/ad08c8 \|doi-access=free \|arxiv=2310.15028 \|bibcode=2024AJ....167...26Y }} This star was previously thought to harbour a directly-imaged planet named Fomalhaut b, before the realization of object as an expanding debris cloud from a planetesimal collision.{{cite journal \|last1=Gáspár \|first1=András \|last2=Rieke \|first2=George H. \|title=New HST data and modeling reveal a massive planetesimal collision around Fomalhaut \|date=April 20, 2020 \|journal=PNAS \|volume=117 \|issue=18 \| pages=9712–9722 \|doi=10.1073/pnas.1912506117 \|pmid=32312810 \|pmc=7211925 \|arxiv=2004.08736 \|bibcode=2020PNAS..117.9712G \|doi-access=free }}
Star with the faintest apparent magnitude with a planet \| MOA-bin-29Lb \| MOA-bin-29L \| Apparent magnitude is 44.61 \|
Closest planet to the celestial north pole (i.e. highest declination) \|TOI-1691 b \|TOI-1691 \|Declination of {{DEC\|+86\|51\|37.23}} \|
Closest planet to the celestial south pole (i.e. lowest declination) \|HD 110082 b \|HD 110082 \|Declination of {{DEC
88\|07\|16}} \|
Star with the highest apparent motion (i.e, proper motion) with a planet \| Barnard planets{{cite journal \|last1=Basant \|first1=Ritvik \|last2=Luque \|first2=Rafael \|display-authors=etal \|date=March 2025 \|title=Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO \|journal=The Astrophysical Journal Letters \|volume=982 \|issue=1\|pages=L1 \|doi=10.3847/2041-8213/adb8d5 \|doi-access=free \|arxiv=2503.08095\|bibcode=2025ApJ...982L...1B }} \| Barnard's Star \| 10.358 arcsec/yr{{Cite web \|title=The Top 20 High Proper Motion - Hipparcos - Cosmos \|url=https://www.cosmos.esa.int/web/hipparcos/high-proper-motion \|access-date=2024-10-02 \|website=www.cosmos.esa.int}} \|As Barnard's Star has the highest apparent motion in the sky, this is currently an absolute record.
Largest angular distance separation from its host star \| COCONUTS-2b \| COCONUTS-2 \| 594 arcseconds \| A candidate planet or brown dwarf around BD+29 5007 has an even larger angular separation of about 935 arcseconds.{{Cite journal \|last=Baig \|first=Sayan \|date=August 2024 \|title=The Ultracool Dwarf Companion catalouge \|url=https://zenodo.org/records/13312178 \|journal=Zenodo \|doi=10.5281/zenodo.13312178 }}
Smallest resolved angular distance separation from its parent star \|Beta Pictoris c \|Beta Pictoris \|0.14 arcseconds \|
Smallest angular distance separation from its parent star \| NGC 6440 X-2 b \| NGC 6440 X-2 \| 0.31 microarcseconds \| Derived from its separation of 0.00255 AU and its distance of ~27 070 light-years (8300 parsecs).{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — NGC 6440 X-2 b. \|url=https://exoplanet.eu/catalog/ngc_6440_x_2_b--612/}}
Star with the largest apparent size (angular diameter) \| Alpha Arietis b \| Hamal \| {{val\|7.006\|0.027}} mas \| Accounted for the limb darkening effect.{{Cite journal \|last1=Baines \|first1=Ellyn K. \|last2=Clark III \|first2=James H. \|last3=Schmitt \|first3=Henrique R. \|last4=Stone \|first4=Jordan M. \|last5=von Braun \|first5=Kaspar \|date=November 2023 \|title=33 New Stellar Angular Diameters from the NPOI, and Nearly 180 NPOI Diameters as an Ensemble \|journal=The Astronomical Journal \|language=en \|volume=166 \|issue=6 \|pages=268 \|doi=10.3847/1538-3881/ad08be \|doi-access=free \|bibcode=2023AJ....166..268B \|issn=1538-3881}} Several stars have a larger angular diameter and were claimed to have candidate planets: Aldebaran ({{val\|20.58\|0.03}} mas),{{cite journal\|doi=10.1051/0004-6361/201526319 \|title=GaiaFGK benchmark stars: Effective temperatures and surface gravities \|journal=Astronomy & Astrophysics \|volume=582 \|pages=A49 \|year=2015 \|last1=Heiter \|first1=U. \|last2=Jofré \|first2=P. \|last3=Gustafsson \|first3=B. \|last4=Korn \|first4=A. J. \|last5=Soubiran \|first5=C. \|last6=Thévenin \|first6=F. \|bibcode=2015A&A...582A..49H \|arxiv=1506.06095 \|s2cid=53391939 }} L2 Puppis ({{val\|17.9\|1.6}} mas){{Cite journal \|last1=Kervella \|first1=P. \|last2=Montargès \|first2=M. \|last3=Ridgway \|first3=S. T. \|last4=Perrin \|first4=G. \|last5=Chesneau \|first5=O. \|last6=Lacour \|first6=S. \|last7=Chiavassa \|first7=A. \|last8=Haubois \|first8=X. \|last9=Gallenne \|first9=A. \|date=2014-04-01 \|title=An edge-on translucent dust disk around the nearest AGB star, L2 Puppis - VLT/NACO spectro-imaging from 1.04 to 4.05 μm and VLTI interferometry \|url=https://www.aanda.org/articles/aa/abs/2014/04/aa23273-13/aa23273-13.html \|journal=Astronomy & Astrophysics \|volume=564 \|pages=A88 \|doi=10.1051/0004-6361/201323273 \|issn=0004-6361 \|arxiv=1404.3189 }}{{cite journal\|title=ALMA observations of the nearby AGB star L2 Puppis - I. Mass of the central star and detection of a candidate planet \|arxiv=1611.06231 \|last1=Kervella \|first1=P. \|last2=Homan\|first2=W.\|last3=Richards\|first3=A. M. S.\|last4=Decin\|first4=L.\|last5=McDonald\|first5=I.\|last6=Montargès\|first6=M.\|last7=Ohnaka\|first7=K.\|year=2016\|doi=10.1051/0004-6361/201629877\|volume=596 \|journal=Astronomy & Astrophysics \|page=A92\|bibcode=2016A&A...596A..92K\|s2cid=55298073 }} and Alpha Centauri A ({{val\|8.314\|0.016}} mas).{{Cite journal \|last1=Kervella \|first1=P. \|last2=Thévenin \|first2=F. \|last3=Ségransan \|first3=D. \|last4=Berthomieu \|first4=G. \|last5=Lopez \|first5=B. \|last6=Morel \|first6=P. \|last7=Provost \|first7=J. \|date=June 2003 \|title=The diameters of alpha Centauri A and B. A comparison of the asteroseismic and VINCI/VLTI views \|url=https://ui.adsabs.harvard.edu/abs/2003A&A...404.1087K/abstract \|journal=Astronomy and Astrophysics \|volume=404 \|pages=1087–1097 \|doi=10.1051/0004-6361:20030570 \|arxiv=astro-ph/0303634 \|bibcode=2003A&A...404.1087K \|issn=0004-6361 }}

class="wikitable sticky-header"

Title

! Planet

! Star

! Data

! Notes

Most distant discovered

| SWEEPS-11 / SWEEPS-04

| SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6

| 27 700 light-years{{cite web |title=Planetary Systems Composite Data |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars |website=NASA Exoplanet Archive |access-date=12 December 2021}}

|Assuming the largest distance from the microlensing light-curve, the planet OGLE-2017-BLG-0364Lb might be more distant, at around 32 600 light-years (10 000 pc).{{Cite journal |last1=Gui |first1=Yuqian |last2=Zang |first2=Weicheng |last3=Zhai |first3=Ruocheng |last4=Ryu |first4=Yoon-Hyun |last5=Udalski |first5=Andrzej |last6=Yang |first6=Hongjing |last7=Han |first7=Cheongho |last8=Mao |first8=Shude |last9=Authors) |first9=(Leading |last10=Albrow |first10=Michael D. |last11=Chung |first11=Sun-Ju |last12=Gould |first12=Andrew |last13=Hwang |first13=Kyu-Ha |last14=Jung |first14=Youn Kil |last15=Shin |first15=In-Gu |date=July 2024|title=Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets |journal=The Astronomical Journal |language=en |volume=168 |issue=2 |pages=49 |doi=10.3847/1538-3881/ad4ce5 |doi-access=free |bibcode=2024AJ....168...49G |issn=1538-3881}}

PSR J0738-4042 at 37 000 ly was shown to be affected by a disk of asteroids but no planets have been detected yet.{{cite news

| url=http://www.science20.com/news_articles/rocks_around_clock_star_psr_j07384042_constantly_pummelled_asteroids-130121

| title=Rocks Around The Clock: Star PSR J0738-4042 Is Constantly Pummelled By Asteroids | work=Science 2.0 | date=2014-02-20

| accessdate=2014-02-23 }}

The most distant potentially habitable planet confirmed is Kepler-1606b, at 2870 light-years distant,{{Cite web|title=Exoplanet-catalog-Exoplanet exploration-Kepler-1606b|date=10 May 2016 |url=https://exoplanets.nasa.gov/exoplanet-catalog/2252/kepler-1606-b/}} although the unconfirmed planet KOI-5889.01 is over 5000 light-years distant.

On 31 March 2022, K2-2016-BLG-0005Lb was reported to be the most distant exoplanet discovered by the Kepler telescope, at 17 000 light-years away.{{cite journal |author=Specht, D. |display-authors=etal|title=Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing|journal=Monthly Notices of the Royal Astronomical Society |year=2023 |volume=520 |issue=4 |pages=6350–6366 |arxiv=2203.16959|doi=10.1093/mnras/stad212 |doi-access=free }}

Among rogue planets, the furthest are very likely extragalactic planets within the lensing system SDSS J1004+4112 at 6.3 billion light-years.{{Cite journal |last1=Bhatiani |first1=Saloni |last2=Dai |first2=Xinyu |last3=Guerras |first3=Eduardo |date=November 2019 |title=Confirmation of Planet-mass Objects in Extragalactic Systems |journal=The Astrophysical Journal |language=en |volume=885 |issue=1 |pages=77 |arxiv=1909.11610 |bibcode=2019ApJ...885...77B |doi=10.3847/1538-4357/ab46ac |issn=0004-637X |doi-access=free}}

Least distant

| {{nowrap|Proxima Centauri b}}

| {{nowrap|Proxima Centauri}}

| 4.25 light-years

| Proxima Centauri b is the closest potentially habitable exoplanet known. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25 000 years), this is an absolute record.

Most distant directly visible

| CT Chamaeleontis b

| CT Chamaeleontis

| 622 light-years

| The resolved likely close to equal mass binary brown dwarf NIRISS-NGC1333-10 AB, the mass of NIRISS-NGC1333-10 B is slightly higher than the deuterium burning limit, is more distant at 978 light-years.{{Cite journal |last1=Langeveld |first1=Adam |last2=Scholz |first2=Aleks |last3=Mužić |first3=Koraljka |last4=Jayawardhana |first4=Ray |last5=Capela |first5=Daniel |last6=Albert |first6=Loïc |last7=Doyon |first7=René |last8=Flagg |first8=Laura |last9=de Furio |first9=Matthew |last10=Johnstone |first10=Doug |last11=Lafrèniere |first11=David |last12=Meyer |first12=Michael |date=2024-08-22 |title=The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-Floating Planets |journal=AJ |volume=168 |issue=4 |page=179 |arxiv=2408.12639 |doi=10.3847/1538-3881/ad6f0c |doi-access=free}}

The disputed planet CVSO 30 c may be more distant, at 1200 light-years away. The candidate planet AT Pyxidis b may also be more distant, at ~1207 light-years away.{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — AT Pyx b. |url=https://exoplanet.eu/catalog/at_pyx_b--10507/}}

Among rogue planets, o005 s41280 is the most distant at 17 300 light-years, followed by A2744-BD-1, at 15 520 light-years away.{{Cite journal |arxiv=2501.16648 |last1=Tu |first1=Zhijun |last2=Wang |first2=Shu |last3=Chen |first3=Xiaodian |last4=Liu |first4=Jifeng |title=Three Brown Dwarfs Masquerading as High-Redshift Galaxies in JWST Observations |journal=The Astrophysical Journal |date=2025 |volume=980 |issue=2 |page=230 |doi=10.3847/1538-4357/adaf9f |doi-access=free |bibcode=2025ApJ...980..230T }}{{Cite journal |arxiv=2308.10900 |last1=Langeroodi |first1=Daniel |last2=Hjorth |first2=Jens |title=Little Red Dots or Brown Dwarfs? NIRSpec Discovery of Three Distant Brown Dwarfs Masquerading as NIRCam-selected Highly Reddened Active Galactic Nuclei |journal=The Astrophysical Journal |date=November 2023 |volume=957 |issue=2 |pages=L27 |doi=10.3847/2041-8213/acfeec |doi-access=free}} As free-floating objects, both of them might not be considered as planets, although their masses might be below 13 M_J.{{cite journal |last1=Basri |first1=Gibor |last2=Brown |first2=E. M. |date=May 2006 |title=Planetesimals to Brown Dwarfs: What is a Planet? |journal=Annual Review of Earth and Planetary Sciences |volume=34 |pages=193–216 |arxiv=astro-ph/0608417 |bibcode=2006AREPS..34..193B |doi=10.1146/annurev.earth.34.031405.125058 |s2cid=119338327}}

Closest directly visible

|Epsilon Indi Ab

|Epsilon Indi

| 12.05 light-years

| {{nowrap|COCONUTS-2b at 35.5 light-years is the}} next closest directly visible.

Star with the brightest apparent magnitude with a planet

| Alpha Arietis b

| Hamal{{Efn|Algieba is mentioned to have a slightly higher magnitude (1.99); however it is the combined magnitude of the system and not of the planet-hosting star, which is 2.37.}}

| Apparent magnitude is 2.005

| Alpha Centauri A (apparent magnitude 0.01) has a directly imaged candidate planet.{{cite journal |last1=Wagner |first1=K. |last2=Boehle |first2=A. |last3=Pathak |first3=P.|last4=Kasper |first4=M.|last5=Arsenault|first5=R. |last6=Jakob|first6=G.|last7=Käufl|first7=U. |last8=Leveratto|first8=S.|last9=Maire|first9=A.-L.|last10=Pantin |first10=E.|last11=Siebenmorgen |first11=R. |last12=Zins|first12=G. |last13=Absil|first13=O. |last14=Ageorges |first14=N. |last15=Apai |first15=D. |last16=Carlotti|first16=A. |last17=Choquet|first17=É.|last18=Delacroix|first18=C.|last19=Dohlen|first19=K.|last20=Duhoux|first20=P.|last21=Forsberg|first21=P.|last22=Fuenteseca|first22=E.|last23=Gutruf|first23=S.|last24=Guyon|first24=O.|last25=Huby|first25=E.|last26=Kampf|first26=D.|last27=Karlsson|first27=M.|last28=Kervella|first28=P.|last29=Kirchbauer|first29=J.-P.|last30=Klupar|first30=P. |last31=Kolb|first31=J.|last32=Mawet|first32=D.|last33=N'Diaye|first33=M.|last34=Orban de Xivry|first34=G.|last35=Quanz|first35=S. P.|last36=Reutlinger|first36=A.|last37=Ruane|first37=G.|last38=Riquelme |first38=M. |last39=Soenke|first39=C.|last40=Sterzik|first40=M.|last41=Vigan|first41=A.|last42=de Zeeuw|first42=T. |display-authors=6 |title=Imaging low-mass planets within the habitable zone of α Centauri |journal=Nature Communications|date=10 February 2021|volume=12|issue=1|page=922|doi=10.1038/s41467-021-21176-6|pmid=33568657|pmc=7876126|doi-access=free|arxiv=2102.05159|bibcode=2021NatCo..12..922W}} [https://www.youtube.com/watch?v=Da2EMPuGu00&feature=youtu.be Kevin Wagner's (lead author of paper?) video of discovery] The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.{{cite press release | title= NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega | url=http://www.nasa.gov/home/hqnews/2013/jan/HQ_13-006_Vega_Asteroid_Belt.html | publisher=Whitney Clavin, NASA | date=8 January 2013 | access-date=4 March 2013}} {{As of|2021}}, a candidate planet around Vega has been detected.{{cite journal |last1=Hurt |first1=Spencer A. |last2=Quinn |first2=Samuel N. |last3=Latham |first3=David W. |last4=Vanderburg |first4=Andrew |last5=Esquerdo |first5=Gilbert A. |last6=Calkins |first6=Michael L. |last7=Berlind |first7=Perry |last8=Angus |first8=Ruth |last9=Latham |first9=Christian A. |last10=Zhou |first10=George |title=A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets |journal=The Astronomical Journal |date=21 January 2021 |volume=161 |issue=4 |page=157 |doi=10.3847/1538-3881/abdec8 |arxiv=2101.08801 |bibcode=2021AJ....161..157H |s2cid=231693198 |doi-access=free }}

Aldebaran (apparent magnitude varies between 0.75 and 0.95) was thought to have a candidate planet, however later studies found the existence of the planet inconclusive.{{cite journal |last=Reichert |first=Katja |arxiv=1903.09157 |title=Precise radial velocities of giant stars XII. Evidence against the proposed planet Aldebaran b |journal=Astronomy & Astrophysics |date=25 March 2019|volume=A22 |page=625 |doi=10.1051/0004-6361/201834028 |bibcode=2019A&A...625A..22R |s2cid=85459692 }} Similarly, Pollux (apparent magnitude = 1.14) and Mirfak (apparent magnitude = 1.806) were claimed to have orbiting planets, both of which have been questioned.{{citation |last1=Ducati |first1=J. R. |title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system |date=2002 |journal=CDS/ADC Collection of Electronic Catalogues |volume=2237 |pages=0 |postscript=. |bibcode=2002yCat.2237....0D |doi=10.26093/cds/vizier |id=VizieR Cat. II/237/colors |doi-access=free}}{{cite conference |last1=Aurière |first1=Michel |last2=Konstantinova-Antova |first2=Renada |display-authors=etal |date=August 2014 |title=Pollux: a stable weak dipolar magnetic field but no planet? |conference=Magnetic Fields throughout Stellar Evolution |volume=302 |pages=359–362 |arxiv=1310.6907 |bibcode=2014IAUS..302..359A |doi=10.1017/S1743921314002476 |book-title=Proceedings of the International Astronomical Union}}{{cite journal |last1=Aurière |first1=M. |last2=Petit |first2=P. |display-authors=etal |date=February 2021 |title=Pollux: A weak dynamo-driven dipolar magnetic field and implications for its probable planet |journal=Astronomy & Astrophysics |volume=646 |issue= |pages=A130 |arxiv=2101.02016 |bibcode=2021A&A...646A.130A |doi=10.1051/0004-6361/202039573}}{{cite journal |bibcode=2012A&A...543A..37L |title=Detection of the 128-day radial velocity variations in the supergiant α Persei. Rotational modulations, pulsations, or a planet? |journal=Astronomy and Astrophysics |volume=543 |pages=A37 |last1=Lee |first1=B. -C |last2=Han |first2=I. |last3=Park |first3=M. -G. |last4=Kim |first4=K. -M. |last5=Mkrtichian |first5=D. E. |year=2012 |arxiv=1205.3840 |doi=10.1051/0004-6361/201118539 |s2cid=118482287 }}

An Earth-mass planet claimed to orbit Alpha Centauri B (apparent magnitude = 1.33) was subsequently refuted.{{cite journal |last1=Rajpaul |first1=Vinesh |arxiv=1510.05598 |title=Ghost in the time series: no planet for Alpha Cen B |date=19 October 2015 |doi=10.1093/mnrasl/slv164 |volume=456 |journal=Monthly Notices of the Royal Astronomical Society: Letters |issue=1 |pages=L6–L10|doi-access=free |bibcode = 2016MNRAS.456L...6R }}

A 2023 study detected 10 luminous point sources around the primary star of Fomalhaut system (apparent magnitude = 1.16), of which the last source may or may not be a planetary-mass companion.{{cite journal |last1=Ygouf |first1=Marie |last2=Beichman |first2=Charles |display-authors=etal |title=Searching for Planets Orbiting Fomalhaut with JWST/NIRCam |journal=The Astronomical Journal |date=October 2023 |volume=167 |issue=1 |page=26 |doi=10.3847/1538-3881/ad08c8 |doi-access=free |arxiv=2310.15028 |bibcode=2024AJ....167...26Y }} This star was previously thought to harbour a directly-imaged planet named Fomalhaut b, before the realization of object as an expanding debris cloud from a planetesimal collision.{{cite journal |last1=Gáspár |first1=András |last2=Rieke |first2=George H. |title=New HST data and modeling reveal a massive planetesimal collision around Fomalhaut |date=April 20, 2020 |journal=PNAS |volume=117 |issue=18 | pages=9712–9722 |doi=10.1073/pnas.1912506117 |pmid=32312810 |pmc=7211925 |arxiv=2004.08736 |bibcode=2020PNAS..117.9712G |doi-access=free }}

Star with the faintest apparent magnitude with a planet

| MOA-bin-29Lb

| MOA-bin-29L

| Apparent magnitude is 44.61

Closest planet to the celestial north pole (i.e. highest declination)

|TOI-1691 b

|TOI-1691

|Declination of {{DEC|+86|51|37.23}}

Closest planet to the celestial south pole (i.e. lowest declination)

|HD 110082 b

|HD 110082

|Declination of {{DEC

88|07|16}}

Star with the highest apparent motion (i.e, proper motion) with a planet

| Barnard planets{{cite journal |last1=Basant |first1=Ritvik |last2=Luque |first2=Rafael |display-authors=etal |date=March 2025 |title=Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO |journal=The Astrophysical Journal Letters |volume=982 |issue=1|pages=L1 |doi=10.3847/2041-8213/adb8d5 |doi-access=free |arxiv=2503.08095|bibcode=2025ApJ...982L...1B }}

| Barnard's Star

| 10.358
arcsec/yr{{Cite web |title=The Top 20 High Proper Motion - Hipparcos - Cosmos |url=https://www.cosmos.esa.int/web/hipparcos/high-proper-motion |access-date=2024-10-02 |website=www.cosmos.esa.int}}

|As Barnard's Star has the highest apparent motion in the sky, this is currently an absolute record.

Largest angular distance separation from its host star

| COCONUTS-2b

| COCONUTS-2

| 594 arcseconds

| A candidate planet or brown dwarf around BD+29 5007 has an even larger angular separation of about 935 arcseconds.{{Cite journal |last=Baig |first=Sayan |date=August 2024 |title=The Ultracool Dwarf Companion catalouge |url=https://zenodo.org/records/13312178 |journal=Zenodo |doi=10.5281/zenodo.13312178 }}

Smallest resolved angular distance separation from its parent star

|Beta Pictoris c

|Beta Pictoris

|0.14 arcseconds

Smallest angular distance separation from its parent star

| NGC 6440 X-2 b

| NGC 6440 X-2

| 0.31 microarcseconds

| Derived from its separation of 0.00255 AU and its distance of ~27 070 light-years (8300 parsecs).{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — NGC 6440 X-2 b. |url=https://exoplanet.eu/catalog/ngc_6440_x_2_b--612/}}

Star with the largest apparent size (angular diameter)

| Alpha Arietis b

| Hamal

| {{val|7.006|0.027}} mas

| Accounted for the limb darkening effect.{{Cite journal |last1=Baines |first1=Ellyn K. |last2=Clark III |first2=James H. |last3=Schmitt |first3=Henrique R. |last4=Stone |first4=Jordan M. |last5=von Braun |first5=Kaspar |date=November 2023 |title=33 New Stellar Angular Diameters from the NPOI, and Nearly 180 NPOI Diameters as an Ensemble |journal=The Astronomical Journal |language=en |volume=166 |issue=6 |pages=268 |doi=10.3847/1538-3881/ad08be |doi-access=free |bibcode=2023AJ....166..268B |issn=1538-3881}}

Several stars have a larger angular diameter and were claimed to have candidate planets: Aldebaran ({{val|20.58|0.03}} mas),{{cite journal|doi=10.1051/0004-6361/201526319 |title=GaiaFGK benchmark stars: Effective temperatures and surface gravities |journal=Astronomy & Astrophysics |volume=582 |pages=A49 |year=2015 |last1=Heiter |first1=U. |last2=Jofré |first2=P. |last3=Gustafsson |first3=B. |last4=Korn |first4=A. J. |last5=Soubiran |first5=C. |last6=Thévenin |first6=F. |bibcode=2015A&A...582A..49H |arxiv=1506.06095 |s2cid=53391939 }} L2 Puppis ({{val|17.9|1.6}} mas){{Cite journal |last1=Kervella |first1=P. |last2=Montargès |first2=M. |last3=Ridgway |first3=S. T. |last4=Perrin |first4=G. |last5=Chesneau |first5=O. |last6=Lacour |first6=S. |last7=Chiavassa |first7=A. |last8=Haubois |first8=X. |last9=Gallenne |first9=A. |date=2014-04-01 |title=An edge-on translucent dust disk around the nearest AGB star, L2 Puppis - VLT/NACO spectro-imaging from 1.04 to 4.05 μm and VLTI interferometry |url=https://www.aanda.org/articles/aa/abs/2014/04/aa23273-13/aa23273-13.html |journal=Astronomy & Astrophysics |volume=564 |pages=A88 |doi=10.1051/0004-6361/201323273 |issn=0004-6361 |arxiv=1404.3189 }}{{cite journal|title=ALMA observations of the nearby AGB star L2 Puppis - I. Mass of the central star and detection of a candidate planet |arxiv=1611.06231 |last1=Kervella |first1=P. |last2=Homan|first2=W.|last3=Richards|first3=A. M. S.|last4=Decin|first4=L.|last5=McDonald|first5=I.|last6=Montargès|first6=M.|last7=Ohnaka|first7=K.|year=2016|doi=10.1051/0004-6361/201629877|volume=596 |journal=Astronomy & Astrophysics |page=A92|bibcode=2016A&A...596A..92K|s2cid=55298073 }} and Alpha Centauri A ({{val|8.314|0.016}} mas).{{Cite journal |last1=Kervella |first1=P. |last2=Thévenin |first2=F. |last3=Ségransan |first3=D. |last4=Berthomieu |first4=G. |last5=Lopez |first5=B. |last6=Morel |first6=P. |last7=Provost |first7=J. |date=June 2003 |title=The diameters of alpha Centauri A and B. A comparison of the asteroseismic and VINCI/VLTI views |url=https://ui.adsabs.harvard.edu/abs/2003A&A...404.1087K/abstract |journal=Astronomy and Astrophysics |volume=404 |pages=1087–1097 |doi=10.1051/0004-6361:20030570 |arxiv=astro-ph/0303634 |bibcode=2003A&A...404.1087K |issn=0004-6361 }}

Planetary characteristics

class="wikitable sticky-header"
Title ! Planet ! Star ! Data ! Notes
{{anchor\|Most massive}} Most massive \| colspan="4" \|The most massive planet is difficult to define due to the blurry line between planets and brown dwarfs. If the borderline is defined as the deuterium fusion threshold (roughly {{Jupiter mass\|13\|link=y}} at solar metallicity{{Cite journal \|last1=Khandelwal \|first1=Akanksha \|last2=Sharma \|first2=Rishikesh \|last3=Chakraborty \|first3=Abhijit \|last4=Chaturvedi \|first4=Priyanka \|last5=Ulmer-Moll \|first5=Solène \|last6=Ciardi \|first6=David R. \|last7=Boyle \|first7=Andrew W. \|last8=Baliwal \|first8=Sanjay \|last9=Bieryla \|first9=Allyson \|last10=Latham \|first10=David W. \|last11=Prasad \|first11=Neelam J. S. S. V. \|last12=Nayak \|first12=Ashirbad \|last13=Lendl \|first13=Monika \|last14=Mordasini \|first14=Christoph \|date=2023-04-01 \|title=Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603 \|url=https://www.aanda.org/articles/aa/abs/2023/04/aa45608-22/aa45608-22.html \|journal=Astronomy & Astrophysics \|language=en \|volume=672 \|pages=L7 \|doi=10.1051/0004-6361/202245608 \|bibcode=2023A&A...672L...7K \|issn=0004-6361 \|arxiv=2303.11841 }}{{Efn\|The deuterium burning limit also depends on the metallicity and abundance of helium. Metal-rich planets, for example, need a lower mass to fuse deuterium.}}), the most massive planets are those with true mass closest to that cutoff; if planets and brown dwarfs are differentiated based on formation, their mass ranges overlap.{{cite journal \|last1=Lecavelier des Etangs \|first1=A. \|last2=Lissauer \|first2=Jack J. \|date=June 2022 \|title=The IAU working definition of an exoplanet \|journal=New Astronomy Reviews \|volume=94 \|issue= \|pages=101641 \|doi=10.1016/j.newar.2022.101641 \|arxiv=2203.09520 \|bibcode=2022NewAR..9401641L}} [https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/ IAU website link]{{cite journal \|last1=Kirkpatrick \|first1=J. Davy \|last2=Marocco \|first2=Federico \|display-authors=etal \|date=April 2024 \|title=The Initial Mass Function Based on the Full-sky 20 pc Census of ~3600 Stars and Brown Dwarfs \|journal=The Astrophysical Journal Supplement Series \|volume=271 \|issue=2 \|pages=55 \|doi=10.3847/1538-4365/ad24e2 \|doi-access=free \|arxiv=2312.03639 \|bibcode=2024ApJS..271...55K}}{{rp\|62}} A candidate for the most massive object that formed in a protoplanetary disk is CWW 89Ab, at about {{Jupiter mass\|36}}. This object is massive enough to have fused deuterium early in its life, but its atmosphere indicates it may have formed via the very high-mass end of the planet formation process.{{Cite journal \|last1=Beatty\|first1=T.G. \|last2=Moreley\|first2=C.V. \|display-authors=et al. \|date=October 2018 \|title=A Significant Overluminosity in the Transiting Brown Dwarf CWW 89Ab \|journal=The Astronomical Journal \|volume=156\|issue=4 \|pages=168 \|doi=10.3847/1538-3881/aad697 \|doi-access=free \|arxiv=1807.11500 \|bibcode=2018AJ....156..168B}}
Most massive in proportion to the mass of the star(s) it revolves around \| Delorme 1 b \| Delorme 1 \| Mass ratio is ~0.034 \| 2M1207 b has a larger ratio to 2M1207 of ~0.2, but the host is a brown dwarf. 2M1207 b may be a sub-brown dwarf instead of a planetary-mass companion.{{Cite journal \|last1=Luhman \|first1=K. L. \|last2=Tremblin \|first2=P. \|last3=Birkmann \|first3=S. M. \|last4=Manjavacas \|first4=E. \|last5=Valenti \|first5=J. \|last6=Alves de Oliveira \|first6=C. \|last7=Beck \|first7=T. L. \|last8=Giardino \|first8=G. \|last9=Lützgendorf \|first9=N. \|last10=Rauscher \|first10=B. J. \|last11=Sirianni \|first11=M. \|date=2023-06-01 \|title=JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B \|journal=The Astrophysical Journal \|volume=949 \|issue=2 \|pages=L36 \|arxiv=2305.18603 \|bibcode=2023ApJ...949L..36L \|doi=10.3847/2041-8213/acd635 \|issn=0004-637X \|doi-access=free}} The planet candidate NSV 1440 b has a higher mass ratio at 0.045 ± 0.002 to its host star, which is a white dwarf. However with a mass near {{val\|30\|ul=Jupiter mass}}, it is likely a companion star that was stripped down to a substellar-mass object.{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — NSV 1440 b. \|url=https://exoplanet.eu/catalog/nsv_1440_b--7307/}}
Most massive in proportion to the mass of the host object it revolves around \|2M1207 b \|2M1207 \|Mass ratio is ~0.2 \|May be a sub-brown dwarf instead of a planetary-mass companion.
Least massive \| PSR J0337+1715 (ABC) b \| PSR J0337+1715 \| {{val\|0.0041\|0.003\|ul=Earth mass}}{{Cite EPE\|name=PSR J0337+1715 b\|access-date=December 30, 2024\|id=10018}} \| The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 {{Earth mass\|link=y}}.{{Cite encyclopedia\|url=https://exoplanet.eu/catalog/\|encyclopedia=Extrasolar Planets Encyclopaedia\|title=The Extrasolar Planet Encyclopaedia — Catalog Listing\|date=11 January 1995 \|access-date=2019-05-04}} As a reference, the mass of Earth's moon is {{val\|0.012\|ul=Earth mass}}.{{cite web \|year=2025 \|website=grc.nasa.gov \|title=Moon \|url=https://www1.grc.nasa.gov/beginners-guide-to-aeronautics/moon/}}
Largest radius \|DH Tauri b \|DH Tauri \|{{Val\|2.7\|0.8}} {{Jupiter radius\|link=y}}{{Cite journal \|last1=Zhou \|first1=Yifan \|last2=Herczeg \|first2=Gregory J. \|last3=Kraus \|first3=Adam L. \|last4=Metchev \|first4=Stanimir \|last5=Cruz \|first5=Kelle L. \|date=2014-02-18 \|title=Accretion Onto Planetary Mass Companions of Low-Mass Young Stars \|url=https://iopscience.iop.org/article/10.1088/2041-8205/783/1/L17 \|journal=The Astrophysical Journal \|volume=783 \|issue=1 \|pages=L17 \|arxiv=1401.6545 \|bibcode=2014ApJ...783L..17Z \|doi=10.1088/2041-8205/783/1/L17 \|issn=2041-8205}} \|Next largest is PDS 70 b with 2.09{{±\|0.23\|0.31}}{{snd}}2.72{{±\|0.15\|0.17}} {{Jupiter radius\|link=y}}.{{Cite journal\|last1=Wang\|first1=Jason J.\|last2=Ginzburg\|first2=Sivan\|last3=Ren\|first3=Bin\|last4=Wallack\|first4=Nicole\|last5=Gao\|first5=Peter\|last6=Mawet\|first6=Dimitri\|last7=Bond\|first7=Charlotte Z.\|last8=Cetre\|first8=Sylvain\|last9=Wizinowich\|first9=Peter\|last10=De Rosa\|first10=Robert J.\|last11=Ruane\|first11=Garreth\|date=2020-05-18\|title=Keck/NIRC2 L{{'}}-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70\|journal=The Astronomical Journal\|volume=159\|issue=6\|pages=263\|doi=10.3847/1538-3881/ab8aef\|arxiv=2004.09597\|bibcode=2020AJ....159..263W\|hdl=2268/254014\|s2cid=216035946\|issn=1538-3881\|doi-access=free }} Proplyd 133-353 is larger at up to 7.4{{±\|0.3}} – 8.0{{±\|1.1}} {{Jupiter radius\|link=y}}.{{Cite journal \|last1=Fang \|first1=Min \|last2=Kim \|first2=Jinyoung Serena \|last3=Pascucci \|first3=Ilaria \|last4=Apai \|first4=Dániel \|last5=Manara \|first5=Carlo Felice \|date=2016-12-12 \|title=A candidate planetary-mass object with a photoevaporating disk in Orion \|journal=The Astrophysical Journal \|volume=833 \|issue=2 \|pages=L16 \|arxiv=1611.09761 \|bibcode=2016ApJ...833L..16F \|doi=10.3847/2041-8213/833/2/L16 \|issn=2041-8213 \|doi-access=free}}{{efn\|name=L/Teff\|Based on the estimated temperature and luminosity.}} It might be considered as a sub-brown dwarf or a rogue planet, with a photoevaporating disk. The largest transiting planet known is XO-6b at 2.17 ± 0.2 {{Jupiter radius\|link=y}}.{{Cite journal \|last=Saha \|first=Suman \|date=2024-09-01 \|title=Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties \|journal=The Astrophysical Journal Supplement Series \|volume=274 \|issue=1 \|pages=13 \|arxiv=2407.20846 \|bibcode=2024ApJS..274...13S \|doi=10.3847/1538-4365/ad6a60 \|doi-access=free \|issn=0067-0049}}
Smallest radius \| Kepler-37b \| Kepler-37 \| {{val\|0.296\|0.037\|ul=Earth radius}} \| The extrasolar planetesimal WD 1145+017 b is smaller.
Most dense \|GP Comae Berenices b \|GP Comae Berenices \|≥185 g/cm³ \|According to the IAU working definition of exoplanets GP Comae Berenices b, being 10 times more massive than Jupiter, is a planet, despite that it might have formed as a white dwarf that was stripped down to a planetary-mass object. For reference, it is a lot denser than osmium at 293 K, the densest naturally occurring stable element on Earth. It is suspected that GP Comae Berenices b might be composed of strange matter based on its density.{{citation\|arxiv=1908.11191\|year=2020\|title=Close-in Exoplanets as Candidates for Strange Quark Matter Objects\|doi=10.3847/1538-4357/ab698b\|last1=Kuerban\|first1=Abudushataer\|last2=Geng\|first2=Jin-Jun\|last3=Huang\|first3=Yong-Feng\|last4=Zong\|first4=Hong-Shi\|last5=Gong\|first5=Hang\|journal=The Astrophysical Journal\|volume=890\|issue=1\|page=41\|bibcode=2020ApJ...890...41K\|s2cid=201671383 \|doi-access=free }} TOI-4603 b is the densest planet which orbits a normal star and is not a potential brown dwarf, with 14.1{{±\|1.7\|1.6}} g/cm³.{{Cite journal \|last1=Khandelwal \|first1=Akanksha \|last2=Sharma \|first2=Rishikesh \|last3=Chakraborty \|first3=Abhijit \|last4=Chaturvedi \|first4=Priyanka \|last5=Ulmer-Moll \|first5=Solène \|last6=Ciardi \|first6=David R. \|last7=Boyle \|first7=Andrew W. \|last8=Baliwal \|first8=Sanjay \|last9=Bieryla \|first9=Allyson \|last10=Latham \|first10=David W. \|last11=Prasad \|first11=Neelam J. S. S. V. \|last12=Nayak \|first12=Ashirbad\|last13=Lendl \|first13=Monika \|last14=Mordasini \|first14=Christoph \|date=2023-04-14 \|title=Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603 \|url=https://www.aanda.org/10.1051/0004-6361/202245608 \|journal=Astronomy & Astrophysics \|volume=672 \|pages=L7 \|arxiv=2303.11841 \|bibcode=2023A&A...672L...7K \|doi=10.1051/0004-6361/202245608 \|issn=0004-6361}}
Least dense \| Kepler-51d \| Kepler-51[http://arxiv.org/abs/1401.2885 Very Low-Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event]: Kento Masuda \| {{Val\|0.0381\|0.0085}} g/cm³ {{Cite journal \|last1=Masuda \|first1=Kento \|last2=Libby-Roberts \|first2=Jessica E. \|last3=Livingston \|first3=John H. \|last4=Stevenson \|first4=Kevin B. \|last5=Gao \|first5=Peter \|last6=Vissapragada \|first6=Shreyas \|last7=Fu \|first7=Guangwei \|last8=Han \|first8=Te \|last9=Greklek-McKeon \|first9=Michael \|last10=Mahadevan \|first10=Suvrath \|last11=Agol \|first11=Eric \|last12=Bello-Arufe \|first12=Aaron \|last13=Berta-Thompson \|first13=Zachory \|last14=Cañas \|first14=Caleb I. \|last15=Chachan \|first15=Yayaati \|date=December 2024 \|title=A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations \|journal=The Astronomical Journal \|language=en \|volume=168 \|issue=6 \|pages=294 \|arxiv=2410.01625 \|doi=10.3847/1538-3881/ad83d3 \|issn=1538-3881 \|doi-access=free\|bibcode=2024AJ....168..294M }} \| Next least dense are the super-Neptune planet WASP-193b with 0.059 ± 0.014 g/cm³{{cite web\|url=https://edition.cnn.com/2024/05/16/world/cotton-candy-exoplanet-discovery-wasp-193b-scn/index.html\|title=Unusual giant planet as fluffy as cotton candy spotted by astronomers\|last=Asmelash\|first=Leah\|website=edition.cnn.com\|publisher=CNN\|date=2024-05-16\|accessdate=2024-05-19}} and the hot Jupiter HAT-P-67b with {{val\|0.060\|0.020\|0.021}} g/cm³,{{cite arXiv \|eprint=2504.13997 \|last1=Wang \|first1=Gavin \|last2=Balmer \|first2=William O. \|last3=Pueyo \|first3=Laurent \|last4=Thorngren \|first4=Daniel \|last5=Schmidt \|first5=Stephen P. \|last6=Wang \|first6=Le-Chris \|last7=Schlaufman \|first7=Kevin C. \|last8=Stefánsson \|first8=Guðmundur \|last9=Rustamkulov \|first9=Zafar \|last10=Sing \|first10=David K. \|title=A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 B \|date=2025 \|class=astro-ph.EP }} tied with Kepler-51 b with {{Val\|0.060\|0.037}} g/cm³. A predicted highly evaporating planet was proposed to orbit the star FU Orionis north with a density of about 0.0042 g/cm³.{{Efn\|Density calculated from the mass of {{Jupiter mass\|~3}} and the radius of {{Jupiter radius\|~9.8}}{{cite journal \|last1=Nayakshin \|first1=Sergei \|last2=Elbakyan \|first2=Vardan \|date=February 2024 \|title=On the origin of accretion bursts in FU Ori \|journal=Monthly Notices of the Royal Astronomical Society \|volume=528 \|issue=2 \|pages=2182–2198 \|doi=10.1093/mnras/stae049 \|doi-access=free \|arxiv=2309.12072 \|bibcode=2024MNRAS.528.2182N }}}}
Highest planetary rotation rate \| Beta Pictoris b \| Beta Pictoris \| 19.9 ± 1.0 km/s \| Value measured at the planetary equator.{{cite journal \|last1=Landman \|first1=R. \|last2=Stolker \|first2=T. \|display-authors=etal \|date=February 2024 \|title=β Pictoris b through the eyes of the upgraded CRIRES+. Atmospheric composition, spin rotation, and radial velocity \|journal=Astronomy & Astrophysics \|volume=682 \|issue= \|pages=A48 \|doi=10.1051/0004-6361/202347846 \|arxiv=2311.13527 \|bibcode=2024A&A...682A..48L }}
Hottest (irradiated planet) \| KELT-9b \| KELT-9 \| 4050 ± 180 K({{Val\|3777\|u=°C}}) \| The candidate planet KOI-2093.03 is hotter, at 6285 K.{{Cite web \|title=Kepler Objects of Interest \|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=cumulative&constraint=koi_disposition+like+'CAN%25' \|archive-url=http://web.archive.org/web/20241007195103/https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=cumulative&constraint=koi_disposition+like+%27CAN%25%27 \|archive-date=2024-10-07 \|access-date=2025-01-04 \|website=exoplanetarchive.ipac.caltech.edu \|language=en}} A candidate planet was suggested to orbit the central star of the Helix Nebula with an equilibrium temperature of 4970 K.{{cite journal \|last1=Iskandarli \|first1=Leyla \|last2=Farihi \|first2=Jay \|display-authors=etal \|date=October 2024 \|title=Novel Constraints on Companions to the Helix Nebula Central Star \|journal=Monthly Notices of the Royal Astronomical Society \|volume= 534\|issue= 4\|pages= 3498–3505\|doi=10.1093/mnras/stae2286 \|doi-access=free \|arxiv=2410.03288 \|bibcode=2024MNRAS.534.3498I }} Kepler-70b and Kepler-70c are often described as the hottest known exoplanets, both at >6800 K (assuming an albedo of 0.1 for both),{{cite journal \|last1=Charpinet \|first1=S. \|last2=Fontaine \|first2=G. \|last3=Brassard \|first3=P. \|last4=Green \|first4=E. M. \|last5=Grootel \|first5=V. Van \|last6=Randall \|first6=S. K. \|last7=Silvotti \|first7=R. \|last8=Baran \|first8=A. S. \|author9=Stensen \|last10=Kawaler \|first10=S. D. \|last11=Telting \|first11=J. H. \| title=A compact system of small planets around a former red-giant star \| journal=Nature \| volume=480 \| issue=7378 \| date=21 December 2011 \| issn=1476-4687 \| doi=10.1038/nature10631 \|pmid=22193103\|pages=496–499\|bibcode = 2011Natur.480..496C \| s2cid=2213885 \|display-authors=1}} but their existence are highly doubtful.{{citation \| first=J. \| last=Krzesinski \| title=Planetary candidates around the pulsating sdB star KIC 5807616 considered doubtful \| journal=Astronomy & Astrophysics \| volume=581 \| date=August 25, 2015 \| pages=A7 \| doi=10.1051/0004-6361/201526346 \| bibcode=2015A&A...581A...7K \| doi-access=free }}{{citation \| first1=A. \| last1=Blokesz \| first2=J. \| last2=Krzesinski \| first3=L. \| last3=Kedziora-Chudczer \| title=Analysis of putative exoplanetary signatures found in light curves of two sdBV stars observed by Kepler \| journal=Astronomy & Astrophysics \| volume=627 \| date=4 July 2019 \| pages=A86 \| doi=10.1051/0004-6361/201835003 \| bibcode=2019A&A...627A..86B \| s2cid=182952925 \| doi-access=free \| arxiv=1906.03321 }}
Hottest (self-luminous) \|GQ Lupi b \|GQ Lupi \|2650 ± 100 K{{Cite journal \|last1=Neuhäuser \|first1=R. \|last2=Mugrauer \|first2=M. \|last3=Seifahrt \|first3=A. \|last4=Schmidt \|first4=T. O. B. \|last5=Vogt \|first5=N. \|date=June 2008 \|title=Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion \|url=http://www.aanda.org/10.1051/0004-6361:20078493 \|journal=Astronomy & Astrophysics \|volume=484 \|issue=1 \|pages=281–291 \|arxiv=0801.2287 \|bibcode=2008A&A...484..281N \|doi=10.1051/0004-6361:20078493 \|issn=0004-6361}} ({{Val\|2377\|u=°C}}) \| GQ Lupi b may be either a massive planet or a brown dwarf.
Coldest \| {{nowrap\|OGLE-2005-BLG-390Lb }} \| {{nowrap\|OGLE-2005-BLG-390L }} \| {{Convert\|50\|K\|C}}{{Cite journal \|last1=Beaulieu \|first1=J. -P. \|last2=Bennett \|first2=D. P. \|last3=Fouqué \|first3=P. \|last4=Williams \|first4=A. \|last5=Dominik \|first5=M. \|last6=Jørgensen \|first6=U. G. \|last7=Kubas \|first7=D. \|last8=Cassan \|first8=A. \|last9=Coutures \|first9=C. \|last10=Greenhill \|first10=J. \|last11=Hill \|first11=K. \|last12=Menzies \|first12=J. \|last13=Sackett \|first13=P. D. \|last14=Albrow \|first14=M. \|last15=Brillant \|first15=S. \|date=2006-01-01 \|title=Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing \|journal=Nature \|volume=439 \|issue=7075 \|pages=437–440 \|doi=10.1038/nature04441 \|issn=0028-0836\|doi-access=free \|pmid=16437108 \|arxiv=astro-ph/0601563 \|bibcode=2006Natur.439..437B }}{{Efn\|This is the calculated equilibrium temperature, assuming an albedo of 0.3}} \| {{nowrap\|The disputed planet Proxima Centauri c}} may be cooler, at {{Convert\|39\|K\|C}}.{{Cite journal \|last1=Damasso \|first1=Mario \|last2=Del Sordo \|first2=Fabio \|last3=Anglada-Escudé \|first3=Guillem \|last4=Giacobbe \|first4=Paolo \|last5=Sozzetti \|first5=Alessandro \|last6=Morbidelli \|first6=Alessandro \|last7=Pojmanski \|first7=Grzegorz \|last8=Barbato \|first8=Domenico \|last9=Butler \|first9=R. Paul \|last10=Jones \|first10=Hugh R. A. \|last11=Hambsch \|first11=Franz-Josef \|last12=Jenkins \|first12=James S. \|last13=López-González \|first13=María José \|last14=Morales \|first14=Nicolás \|last15=Peña Rojas \|first15=Pablo A. \|date=2020-01-01 \|title=A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU \|journal=Science Advances \|volume=6 \|issue=3 \|pages=eaax7467 \|doi=10.1126/sciadv.aax7467\|doi-access=free \|pmid=31998838 \|pmc=6962037 \|bibcode=2020SciA....6.7467D }}
Fastest jetstream wind \| WASP-127b \| WASP-127 \| 33 000 km/h (9200 m/s){{Cite web \|date=2024-10-01 \|title=Detection of the resolved signatures of a supersonic equatorial jet and cool poles in a hot planet \|url=https://www.eso.org/public/archives/releases/sciencepapers/eso2502/eso2502a.pdf \|website=eso.org}} \|
Strongest magnetic field \| Tau Boötis b \| Tau Boötis \| {{val\|117\|38}} G{{Efn\|Calculated assuming a ratio of 0.2% for the amount of total energy emitted in the Ca II K band.{{Cite journal\|last1=Cauley\|first1=P. Wilson\|last2=Shkolnik\|first2=Evgenya L.\|last3=Llama\|first3=Joe\|last4=Lanza\|first4=Antonino F.\|date=Dec 2019\|title=Magnetic field strengths of hot Jupiters from signals of star-planet interactions\|journal=Nature Astronomy\|volume=3\|issue=12\|pages=1128–1134\|doi=10.1038/s41550-019-0840-x\|arxiv=1907.09068\|bibcode=2019NatAs...3.1128C\|s2cid=198147426\|issn=2397-3366}}}} \| For comparison, the field strength of Jupiter is 4.17 G.{{Cite journal \|last1=Connerney \|first1=J. E. P. \|last2=Kotsiaros \|first2=S. \|last3=Oliversen \|first3=R. J. \|last4=Espley \|first4=J. R. \|last5=Joergensen \|first5=J. L. \|last6=Joergensen \|first6=P. S. \|last7=Merayo \|first7=J. M. G. \|last8=Herceg \|first8=M. \|last9=Bloxham \|first9=J. \|last10=Moore \|first10=K. M. \|last11=Bolton \|first11=S. J. \|last12=Levin \|first12=S. M. \|date=May 26, 2017 \|title=A New Model of Jupiter's Magnetic Field From Juno's First Nine Orbits \|url=http://orbit.dtu.dk/ws/files/147221632/Connerney_et_al_2018_Geophysical_Research_Letters.pdf \|url-status=live \|journal=Geophysical Research Letters \|language=en \|volume=45 \|issue=6 \|pages=2590–2596 \|bibcode=2018GeoRL..45.2590C \|doi=10.1002/2018GL077312 \|archive-url=https://ghostarchive.org/archive/20221009/http://orbit.dtu.dk/ws/files/147221632/Connerney_et_al_2018_Geophysical_Research_Letters.pdf \|archive-date=October 9, 2022 \|doi-access=free}} The magnetic field of SIMP J013656.5+093347 is stronger at ~3200 G.{{Cite journal\|last1=Kao\|first1=Melodie M.\|last2=Hallinan\|first2=Gregg\|last3=Pineda\|first3=J. Sebastian\|last4=Stevenson\|first4=David\|last5=Burgasser\|first5=Adam\|date=August 2018\|title=The Strongest Magnetic Fields on the Coolest Brown Dwarfs\|journal=Astrophysical Journal Supplement Series\|language=en\|volume=237\|issue=2\|pages=25\|doi=10.3847/1538-4365/aac2d5\|arxiv=1808.02485 \|issn=0067-0049 \|bibcode=2018ApJS..237...25K \|doi-access=free }} As a free-floating object, it might not be considered as a planet.
Highest albedo \| LTT 9779 b \| LTT 9779 \| 0.79 ± 0.15 \| This is value for the western dayside region, with the overall albedo of dayside being 0.50 ± 0.07.{{Cite web \|title=Highly Reflective White Clouds On The Western Dayside Of An Exo-Neptune \|url=https://astrobiology.com/2025/01/highly-reflective-white-clouds-on-the-western-dayside-of-an-exo-neptune.html \|access-date=2025-02-01 \|website=astrobiology.com\|date=28 January 2025 }} For comparison, Earth is 0.3 and Venus is 0.76.
Lowest albedo \| {{nowrap\|TrES-2b}} \| {{nowrap\|GSC 03549-02811}} \| Geometric albedo {{nowrap\|< 1%}}{{cite journal\|author=David M. Kipping \|display-authors=etal \|title=Detection of visible light from the darkest world \|journal=Monthly Notices of the Royal Astronomical Society \|doi=10.1111/j.1745-3933.2011.01127.x \|arxiv=1108.2297 \|bibcode=2011MNRAS.417L..88K \|volume=417 \|issue=1 \|pages=L88–L92 \|year=2011 \|doi-access=free \|s2cid=119287494}} \| Best-fit model for albedo gives 0.04% (0.0004).
Youngest \|DH Tauri b \|DH Tauri \| {{val\|0.7\|0.3\|0.2}} Myr{{Cite journal \|last1=Xuan \|first1=Jerry W. \|last2=Hsu \|first2=Chih-Chun \|last3=Finnerty \|first3=Luke \|last4=Wang \|first4=Jason \|last5=Ruffio \|first5=Jean-Baptiste \|last6=Zhang \|first6=Yapeng \|last7=Knutson \|first7=Heather A. \|last8=Mawet \|first8=Dimitri \|last9=Mamajek \|first9=Eric E. \|last10=Inglis \|first10=Julie \|last11=Wallack \|first11=Nicole L. \|last12=Bryan \|first12=Marta L. \|last13=Blake \|first13=Geoffrey A. \|last14=Mollière \|first14=Paul \|last15=Hejazi \|first15=Neda \|date=2024-07-01 \|title=Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of ~10–30 M Jup Companions \|journal=The Astrophysical Journal \|volume=970 \|issue=1 \|page=71 \|arxiv=2405.13128 \|bibcode=2024ApJ...970...71X \|doi=10.3847/1538-4357/ad4796 \|doi-access=free \|issn=0004-637X}} \|The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.{{Cite encyclopedia \|title=The Extrasolar Planet Encyclopaedia — Proplyd 133-353 \|encyclopedia=Extrasolar Planets Encyclopaedia \|url=https://exoplanet.eu/catalog/proplyd_133_353--4078/ \|access-date=2019-03-30}} However, as a free-floating planet, it does not meet the IAU's working definition of a planet. 2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr, but fails the mass ratio criterion of the IAU working definition of an exoplanet; the mass ratio with the primary is larger than the L4/L5 limit of stability ≈ 1/25{{Cite journal \|last1=Lecavelier des Etangs \|first1=A. \|last2=Lissauer \|first2=Jack J. \|date=2022-06-01 \|title=The IAU working definition of an exoplanet \|url=https://linkinghub.elsevier.com/retrieve/pii/S138764732200001X \|journal=New Astronomy Reviews \|language=en \|volume=94 \|pages=101641 \|arxiv=2203.09520 \|bibcode=2022NewAR..9401641L \|doi=10.1016/j.newar.2022.101641}} and the companion is 'more likely to have been produced by cloud core fragmentation' (similar to a star).{{Cite journal \|last1=Todorov \|first1=K. \|last2=Luhman \|first2=K. L. \|last3=McLeod \|first3=K. K. \|date=2010-05-01 \|title=Discovery of a Planetary-Mass Companion to a Brown Dwarf in Taurus \|url=https://iopscience.iop.org/article/10.1088/2041-8205/714/1/L84 \|journal=The Astrophysical Journal \|volume=714 \|issue=1 \|pages=L84–L88 \|arxiv=1004.0539 \|bibcode=2010ApJ...714L..84T \|doi=10.1088/2041-8205/714/1/L84 \|issn=2041-8205}} Two planetary candidates proposed to orbit IRS 63 are at ≲0.5 Myr.{{cite journal \|arxiv=2010.03657 \|doi=10.1038/s41586-020-2779-6 \|title=Four annular structures in a protostellar disk less than 500,000 years old \|date=2020 \|last1=Segura-Cox \|first1=Dominique M. \|last2=Schmiedeke \|first2=Anika \|last3=Pineda \|first3=Jaime E. \|last4=Stephens \|first4=Ian W. \|last5=Fernández-López \|first5=Manuel \|last6=Looney \|first6=Leslie W. \|last7=Caselli \|first7=Paola \|last8=Li \|first8=Zhi-Yun \|last9=Mundy \|first9=Lee G. \|last10=Kwon \|first10=Woojin \|last11=Harris \|first11=Robert J. \|journal=Nature \|volume=586 \|issue=7828 \|pages=228–231 \|pmid=33028998 }} IRAS 04125+2902 b is the youngest transiting planet at an age of ~3 Myr.{{Cite journal \|last1=Barber \|first1=Madyson G. \|last2=Mann \|first2=Andrew W. \|last3=Vanderburg \|first3=Andrew \|last4=Krolikowski \|first4=Daniel \|last5=Kraus \|first5=Adam \|last6=Ansdell \|first6=Megan \|last7=Pearce \|first7=Logan \|last8=Mace \|first8=Gregory N. \|last9=Andrews \|first9=Sean M. \|last10=Boyle \|first10=Andrew W. \|last11=Collins \|first11=Karen A. \|last12=De Furio \|first12=Matthew \|last13=Dragomir \|first13=Diana \|last14=Espaillat \|first14=Catherine \|last15=Feinstein \|first15=Adina D. \|date=November 2024 \|title=A giant planet transiting a 3-Myr protostar with a misaligned disk \|url=https://www.nature.com/articles/s41586-024-08123-3 \|journal=Nature \|language=en \|volume=635 \|issue=8039 \|pages=574–577 \|doi=10.1038/s41586-024-08123-3 \|pmid=39567788 \|arxiv=2411.18683 \|bibcode=2024Natur.635..574B \|issn=1476-4687}} CI Tauri c would be the youngest radial velocity planet at an age of 2–3 Myr, if confirmed.{{Cite journal \|last1=Manick \|first1=R. \|last2=Sousa \|first2=A. P. \|last3=Bouvier \|first3=J. \|last4=Almenara \|first4=J. M. \|last5=Rebull \|first5=L. \|last6=Bayo \|first6=A. \|last7=Carmona \|first7=A. \|last8=Martioli \|first8=E. \|last9=Venuti \|first9=L. \|last10=Pantolmos \|first10=G. \|last11=Kóspál \|first11=á. \|last12=Zanni \|first12=C. \|last13=Bonfils \|first13=X. \|last14=Moutou \|first14=C. \|last15=Delfosse \|first15=X. \|date=June 2024 \|title=Long-period modulation of the classical T Tauri star CI Tau: Evidence for an eccentric close-in massive planet at 0.17 au \|url=https://www.aanda.org/10.1051/0004-6361/202348258 \|journal=Astronomy & Astrophysics \|volume=686 \|pages=A249 \|arxiv=2403.03706 \|bibcode=2024A&A...686A.249M \|doi=10.1051/0004-6361/202348258 \|issn=0004-6361}}{{efn\|1=Most sources like the NASA Exoplanet Archive and exoplanet.eu already accept it as confirmed.{{cite web \|url=https://exoplanetarchive.ipac.caltech.edu/overview/CI%20Tau \|title=CI Tau \|website=NASA Exoplanet Archive \|access-date=29 March 2024}}{{cite EPE\|title=CI Tau c\|id=10725}}}}
Oldest \| TOI-157 b \| TOI-157 \| {{Val\|12.82\|0.73\|1.40\|ul=}} Gyr{{Cite journal \|last1=Nielsen \|first1=L. D. \|last2=Brahm \|first2=R. \|last3=Bouchy \|first3=F. \|last4=Espinoza \|first4=N. \|last5=Turner \|first5=O. \|last6=Rappaport \|first6=S. \|last7=Pearce \|first7=L. \|last8=Ricker \|first8=G. \|last9=Vanderspek \|first9=R. \|last10=Latham \|first10=D. W. \|last11=Seager \|first11=S. \|last12=Winn \|first12=J. N. \|last13=Jenkins \|first13=J. M. \|last14=Acton \|first14=J. S. \|last15=Bakos \|first15=G. \|date=July 2020 \|title=Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b \|url=https://www.aanda.org/10.1051/0004-6361/202037941 \|journal=Astronomy & Astrophysics \|volume=639 \|pages=A76 \|arxiv=2003.05932 \|bibcode=2020A&A...639A..76N \|doi=10.1051/0004-6361/202037941 \|issn=0004-6361}} \| The currently accepted age of the universe is around 13.8 billion years. Could alternatively be PSR B1620-26 b with 11.2–12.7 Gyr.{{Cite journal \|last1=Lacki \|first1=Brian C. \|last2=Brzycki \|first2=Bryan \|last3=Croft \|first3=Steve \|last4=Czech \|first4=Daniel \|last5=DeBoer \|first5=David \|last6=DeMarines \|first6=Julia \|last7=Gajjar \|first7=Vishal \|last8=Isaacson \|first8=Howard \|last9=Lebofsky \|first9=Matt \|last10=MacMahon \|first10=David H. E. \|last11=Price \|first11=Danny C. \|last12=Sheikh \|first12=Sofia Z. \|last13=Siemion \|first13=Andrew P. V. \|last14=Drew \|first14=Jamie \|last15=Worden \|first15=S. Pete \|date=2021-12-01 \|title=One of Everything: The Breakthrough Listen Exotica Catalog \|journal=The Astrophysical Journal Supplement Series \|volume=257 \|issue=2 \|pages=42 \|arxiv=2006.11304 \|bibcode=2021ApJS..257...42L \|doi=10.3847/1538-4365/ac168a \|issn=0067-0049 \|doi-access=free}} Two disproven planets had been thought to orbit the star HIP 11952,{{Cite journal\|bibcode = 2014A&A...562A.129J\|title = No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044\|last1 = Jones\|first1 = M. I.\|last2 = Jenkins\|first2 = J. S.\|journal = Astronomy and Astrophysics\|year = 2014\|volume = 562\|pages = A129\|doi = 10.1051/0004-6361/201322132\|arxiv = 1401.0517\|s2cid = 55365608}} whose age is {{Val\|12.8\|2.6}} Gyr.{{cite encyclopedia \| url=http://exoplanet.eu/star.php?st=HIP+11952 \| archive-url=https://web.archive.org/web/20120505093906/http://exoplanet.eu/star.php?st=HIP+11952 \| url-status=dead \| archive-date=May 5, 2012 \| title=Notes for Star HIP 11952 \| date=23 March 2012 \| access-date=March 29, 2012 \| encyclopedia=Extrasolar Planets Encyclopaedia \| author=Schneider, Jean}} The star HE 1523-0901 might be older at 13.2 Gyr {{cite journal \|last1= Frebel\|first1=A. \|display-authors=etal \|date=2007 \|journal=The Astrophysical Journal \|volume=660 \|issue=2 \|page=L117 \|title=Discovery of HE 1523–0901, a Strongly r-Process-enhanced Metal-poor Star with Detected Uranium \|arxiv=astro-ph/0703414 \|bibcode=2007ApJ...660L.117F \|doi=10.1086/518122 \|s2cid=17533424 }} and has a candidate planet or brown dwarf.{{citation\|arxiv=1509.05344\|year=2015\|title=The role of binaries in the enrichment of the early Galactic halo. I. r-process-enhanced metal-poor stars\|doi=10.1051/0004-6361/201526812 \|last1=Hansen \|first1=T. T. \|last2=Andersen \|first2=J. \|last3=Nordström \|first3=B. \|last4=Beers \|first4=T. C. \|last5=Yoon \|first5=J. \|last6=Buchhave \|first6=L. A. \|journal=Astronomy & Astrophysics \|volume=583 \|pages=A49 \|bibcode=2015A&A...583A..49H }}

class="wikitable sticky-header"

Title

! Planet

! Star

! Data

! Notes

{{anchor|Most massive}} Most massive

| colspan="4" |The most massive planet is difficult to define due to the blurry line between planets and brown dwarfs. If the borderline is defined as the deuterium fusion threshold (roughly {{Jupiter mass|13|link=y}} at solar metallicity{{Cite journal |last1=Khandelwal |first1=Akanksha |last2=Sharma |first2=Rishikesh |last3=Chakraborty |first3=Abhijit |last4=Chaturvedi |first4=Priyanka |last5=Ulmer-Moll |first5=Solène |last6=Ciardi |first6=David R. |last7=Boyle |first7=Andrew W. |last8=Baliwal |first8=Sanjay |last9=Bieryla |first9=Allyson |last10=Latham |first10=David W. |last11=Prasad |first11=Neelam J. S. S. V. |last12=Nayak |first12=Ashirbad |last13=Lendl |first13=Monika |last14=Mordasini |first14=Christoph |date=2023-04-01 |title=Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603 |url=https://www.aanda.org/articles/aa/abs/2023/04/aa45608-22/aa45608-22.html |journal=Astronomy & Astrophysics |language=en |volume=672 |pages=L7 |doi=10.1051/0004-6361/202245608 |bibcode=2023A&A...672L...7K |issn=0004-6361 |arxiv=2303.11841 }}{{Efn|The deuterium burning limit also depends on the metallicity and abundance of helium. Metal-rich planets, for example, need a lower mass to fuse deuterium.}}), the most massive planets are those with true mass closest to that cutoff; if planets and brown dwarfs are differentiated based on formation, their mass ranges overlap.{{cite journal |last1=Lecavelier des Etangs |first1=A. |last2=Lissauer |first2=Jack J. |date=June 2022 |title=The IAU working definition of an exoplanet |journal=New Astronomy Reviews |volume=94 |issue= |pages=101641 |doi=10.1016/j.newar.2022.101641 |arxiv=2203.09520 |bibcode=2022NewAR..9401641L}} [https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/ IAU website link]{{cite journal |last1=Kirkpatrick |first1=J. Davy |last2=Marocco |first2=Federico |display-authors=etal |date=April 2024 |title=The Initial Mass Function Based on the Full-sky 20 pc Census of ~3600 Stars and Brown Dwarfs |journal=The Astrophysical Journal Supplement Series |volume=271 |issue=2 |pages=55 |doi=10.3847/1538-4365/ad24e2 |doi-access=free |arxiv=2312.03639 |bibcode=2024ApJS..271...55K}}{{rp|62}} A candidate for the most massive object that formed in a protoplanetary disk is CWW 89Ab, at about {{Jupiter mass|36}}. This object is massive enough to have fused deuterium early in its life, but its atmosphere indicates it may have formed via the very high-mass end of the planet formation process.{{Cite journal |last1=Beatty|first1=T.G. |last2=Moreley|first2=C.V. |display-authors=et al. |date=October 2018 |title=A Significant Overluminosity in the Transiting Brown Dwarf CWW 89Ab |journal=The Astronomical Journal |volume=156|issue=4 |pages=168 |doi=10.3847/1538-3881/aad697 |doi-access=free |arxiv=1807.11500 |bibcode=2018AJ....156..168B}}

Most massive in proportion to the mass of the star(s) it revolves around

| Delorme 1 b

| Delorme 1

| Mass ratio is ~0.034

| 2M1207 b has a larger ratio to 2M1207 of ~0.2, but the host is a brown dwarf. 2M1207 b may be a sub-brown dwarf instead of a planetary-mass companion.{{Cite journal |last1=Luhman |first1=K. L. |last2=Tremblin |first2=P. |last3=Birkmann |first3=S. M. |last4=Manjavacas |first4=E. |last5=Valenti |first5=J. |last6=Alves de Oliveira |first6=C. |last7=Beck |first7=T. L. |last8=Giardino |first8=G. |last9=Lützgendorf |first9=N. |last10=Rauscher |first10=B. J. |last11=Sirianni |first11=M. |date=2023-06-01 |title=JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B |journal=The Astrophysical Journal |volume=949 |issue=2 |pages=L36 |arxiv=2305.18603 |bibcode=2023ApJ...949L..36L |doi=10.3847/2041-8213/acd635 |issn=0004-637X |doi-access=free}}

The planet candidate NSV 1440 b has a higher mass ratio at 0.045 ± 0.002 to its host star, which is a white dwarf. However with a mass near {{val|30|ul=Jupiter mass}}, it is likely a companion star that was stripped down to a substellar-mass object.{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — NSV 1440 b. |url=https://exoplanet.eu/catalog/nsv_1440_b--7307/}}

Most massive in proportion to the mass of the host object it revolves around

|2M1207 b

|2M1207

|Mass ratio is ~0.2

|May be a sub-brown dwarf instead of a planetary-mass companion.

Least massive

| PSR J0337+1715 (ABC) b

| PSR J0337+1715

| {{val|0.0041|0.003|ul=Earth mass}}{{Cite EPE|name=PSR J0337+1715 b|access-date=December 30, 2024|id=10018}}

| The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 {{Earth mass|link=y}}.{{Cite encyclopedia|url=https://exoplanet.eu/catalog/|encyclopedia=Extrasolar Planets Encyclopaedia|title=The Extrasolar Planet Encyclopaedia — Catalog Listing|date=11 January 1995 |access-date=2019-05-04}}

As a reference, the mass of Earth's moon is {{val|0.012|ul=Earth mass}}.{{cite web |year=2025 |website=grc.nasa.gov |title=Moon |url=https://www1.grc.nasa.gov/beginners-guide-to-aeronautics/moon/}}

Largest radius

|DH Tauri b

|DH Tauri

|{{Val|2.7|0.8}} {{Jupiter radius|link=y}}{{Cite journal |last1=Zhou |first1=Yifan |last2=Herczeg |first2=Gregory J. |last3=Kraus |first3=Adam L. |last4=Metchev |first4=Stanimir |last5=Cruz |first5=Kelle L. |date=2014-02-18 |title=Accretion Onto Planetary Mass Companions of Low-Mass Young Stars |url=https://iopscience.iop.org/article/10.1088/2041-8205/783/1/L17 |journal=The Astrophysical Journal |volume=783 |issue=1 |pages=L17 |arxiv=1401.6545 |bibcode=2014ApJ...783L..17Z |doi=10.1088/2041-8205/783/1/L17 |issn=2041-8205}}

|Next largest is PDS 70 b with 2.09{{±|0.23|0.31}}{{snd}}2.72{{±|0.15|0.17}} {{Jupiter radius|link=y}}.{{Cite journal|last1=Wang|first1=Jason J.|last2=Ginzburg|first2=Sivan|last3=Ren|first3=Bin|last4=Wallack|first4=Nicole|last5=Gao|first5=Peter|last6=Mawet|first6=Dimitri|last7=Bond|first7=Charlotte Z.|last8=Cetre|first8=Sylvain|last9=Wizinowich|first9=Peter|last10=De Rosa|first10=Robert J.|last11=Ruane|first11=Garreth|date=2020-05-18|title=Keck/NIRC2 L{{'}}-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70|journal=The Astronomical Journal|volume=159|issue=6|pages=263|doi=10.3847/1538-3881/ab8aef|arxiv=2004.09597|bibcode=2020AJ....159..263W|hdl=2268/254014|s2cid=216035946|issn=1538-3881|doi-access=free }}

Proplyd 133-353 is larger at up to 7.4{{±|0.3}} – 8.0{{±|1.1}} {{Jupiter radius|link=y}}.{{Cite journal |last1=Fang |first1=Min |last2=Kim |first2=Jinyoung Serena |last3=Pascucci |first3=Ilaria |last4=Apai |first4=Dániel |last5=Manara |first5=Carlo Felice |date=2016-12-12 |title=A candidate planetary-mass object with a photoevaporating disk in Orion |journal=The Astrophysical Journal |volume=833 |issue=2 |pages=L16 |arxiv=1611.09761 |bibcode=2016ApJ...833L..16F |doi=10.3847/2041-8213/833/2/L16 |issn=2041-8213 |doi-access=free}}{{efn|name=L/Teff|Based on the estimated temperature and luminosity.}} It might be considered as a sub-brown dwarf or a rogue planet, with a photoevaporating disk.

The largest transiting planet known is XO-6b at 2.17 ± 0.2 {{Jupiter radius|link=y}}.{{Cite journal |last=Saha |first=Suman |date=2024-09-01 |title=Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties |journal=The Astrophysical Journal Supplement Series |volume=274 |issue=1 |pages=13 |arxiv=2407.20846 |bibcode=2024ApJS..274...13S |doi=10.3847/1538-4365/ad6a60 |doi-access=free |issn=0067-0049}}

Smallest radius

| Kepler-37b

| Kepler-37

| {{val|0.296|0.037|ul=Earth radius}}

| The extrasolar planetesimal WD 1145+017 b is smaller.

Most dense

|GP Comae Berenices b

|GP Comae Berenices

|≥185 g/cm³

|According to the IAU working definition of exoplanets GP Comae Berenices b, being 10 times more massive than Jupiter, is a planet, despite that it might have formed as a white dwarf that was stripped down to a planetary-mass object. For reference, it is a lot denser than osmium at 293 K, the densest naturally occurring stable element on Earth. It is suspected that GP Comae Berenices b might be composed of strange matter based on its density.{{citation|arxiv=1908.11191|year=2020|title=Close-in Exoplanets as Candidates for Strange Quark Matter Objects|doi=10.3847/1538-4357/ab698b|last1=Kuerban|first1=Abudushataer|last2=Geng|first2=Jin-Jun|last3=Huang|first3=Yong-Feng|last4=Zong|first4=Hong-Shi|last5=Gong|first5=Hang|journal=The Astrophysical Journal|volume=890|issue=1|page=41|bibcode=2020ApJ...890...41K|s2cid=201671383 |doi-access=free }}

TOI-4603 b is the densest planet which orbits a normal star and is not a potential brown dwarf, with 14.1{{±|1.7|1.6}} g/cm³.{{Cite journal |last1=Khandelwal |first1=Akanksha |last2=Sharma |first2=Rishikesh |last3=Chakraborty |first3=Abhijit |last4=Chaturvedi |first4=Priyanka |last5=Ulmer-Moll |first5=Solène |last6=Ciardi |first6=David R. |last7=Boyle |first7=Andrew W. |last8=Baliwal |first8=Sanjay |last9=Bieryla |first9=Allyson |last10=Latham |first10=David W. |last11=Prasad |first11=Neelam J. S. S. V. |last12=Nayak |first12=Ashirbad|last13=Lendl |first13=Monika |last14=Mordasini |first14=Christoph |date=2023-04-14 |title=Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603 |url=https://www.aanda.org/10.1051/0004-6361/202245608 |journal=Astronomy & Astrophysics |volume=672 |pages=L7 |arxiv=2303.11841 |bibcode=2023A&A...672L...7K |doi=10.1051/0004-6361/202245608 |issn=0004-6361}}

Least dense

| Kepler-51d

| Kepler-51[http://arxiv.org/abs/1401.2885 Very Low-Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event]: Kento Masuda

| {{Val|0.0381|0.0085}} g/cm³ {{Cite journal |last1=Masuda |first1=Kento |last2=Libby-Roberts |first2=Jessica E. |last3=Livingston |first3=John H. |last4=Stevenson |first4=Kevin B. |last5=Gao |first5=Peter |last6=Vissapragada |first6=Shreyas |last7=Fu |first7=Guangwei |last8=Han |first8=Te |last9=Greklek-McKeon |first9=Michael |last10=Mahadevan |first10=Suvrath |last11=Agol |first11=Eric |last12=Bello-Arufe |first12=Aaron |last13=Berta-Thompson |first13=Zachory |last14=Cañas |first14=Caleb I. |last15=Chachan |first15=Yayaati |date=December 2024 |title=A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations |journal=The Astronomical Journal |language=en |volume=168 |issue=6 |pages=294 |arxiv=2410.01625 |doi=10.3847/1538-3881/ad83d3 |issn=1538-3881 |doi-access=free|bibcode=2024AJ....168..294M }}

| Next least dense are the super-Neptune planet WASP-193b with 0.059 ± 0.014 g/cm³{{cite web|url=https://edition.cnn.com/2024/05/16/world/cotton-candy-exoplanet-discovery-wasp-193b-scn/index.html|title=Unusual giant planet as fluffy as cotton candy spotted by astronomers|last=Asmelash|first=Leah|website=edition.cnn.com|publisher=CNN|date=2024-05-16|accessdate=2024-05-19}} and the hot Jupiter HAT-P-67b with {{val|0.060|0.020|0.021}} g/cm³,{{cite arXiv |eprint=2504.13997 |last1=Wang |first1=Gavin |last2=Balmer |first2=William O. |last3=Pueyo |first3=Laurent |last4=Thorngren |first4=Daniel |last5=Schmidt |first5=Stephen P. |last6=Wang |first6=Le-Chris |last7=Schlaufman |first7=Kevin C. |last8=Stefánsson |first8=Guðmundur |last9=Rustamkulov |first9=Zafar |last10=Sing |first10=David K. |title=A Revised Density Estimate for the Largest Known Exoplanet, HAT-P-67 B |date=2025 |class=astro-ph.EP }} tied with Kepler-51 b with {{Val|0.060|0.037}} g/cm³.

A predicted highly evaporating planet was proposed to orbit the star FU Orionis north with a density of about 0.0042 g/cm³.{{Efn|Density calculated from the mass of {{Jupiter mass|~3}} and the radius of {{Jupiter radius|~9.8}}{{cite journal |last1=Nayakshin |first1=Sergei |last2=Elbakyan |first2=Vardan |date=February 2024 |title=On the origin of accretion bursts in FU Ori |journal=Monthly Notices of the Royal Astronomical Society |volume=528 |issue=2 |pages=2182–2198 |doi=10.1093/mnras/stae049 |doi-access=free |arxiv=2309.12072 |bibcode=2024MNRAS.528.2182N }}}}

Highest planetary rotation rate

| Beta Pictoris b

| Beta Pictoris

| 19.9 ± 1.0 km/s

| Value measured at the planetary equator.{{cite journal |last1=Landman |first1=R. |last2=Stolker |first2=T. |display-authors=etal |date=February 2024 |title=β Pictoris b through the eyes of the upgraded CRIRES+. Atmospheric composition, spin rotation, and radial velocity |journal=Astronomy & Astrophysics |volume=682 |issue= |pages=A48 |doi=10.1051/0004-6361/202347846 |arxiv=2311.13527 |bibcode=2024A&A...682A..48L }}

Hottest (irradiated planet)

| KELT-9b

| KELT-9

| 4050 ± 180 K({{Val|3777|u=°C}})

| The candidate planet KOI-2093.03 is hotter, at 6285 K.{{Cite web |title=Kepler Objects of Interest |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=cumulative&constraint=koi_disposition+like+'CAN%25' |archive-url=http://web.archive.org/web/20241007195103/https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=cumulative&constraint=koi_disposition+like+%27CAN%25%27 |archive-date=2024-10-07 |access-date=2025-01-04 |website=exoplanetarchive.ipac.caltech.edu |language=en}}

A candidate planet was suggested to orbit the central star of the Helix Nebula with an equilibrium temperature of 4970 K.{{cite journal |last1=Iskandarli |first1=Leyla |last2=Farihi |first2=Jay |display-authors=etal |date=October 2024 |title=Novel Constraints on Companions to the Helix Nebula Central Star |journal=Monthly Notices of the Royal Astronomical Society |volume= 534|issue= 4|pages= 3498–3505|doi=10.1093/mnras/stae2286 |doi-access=free |arxiv=2410.03288 |bibcode=2024MNRAS.534.3498I }}

Kepler-70b and Kepler-70c are often described as the hottest known exoplanets, both at >6800 K (assuming an albedo of 0.1 for both),{{cite journal |last1=Charpinet |first1=S. |last2=Fontaine |first2=G. |last3=Brassard |first3=P. |last4=Green |first4=E. M. |last5=Grootel |first5=V. Van |last6=Randall |first6=S. K. |last7=Silvotti |first7=R. |last8=Baran |first8=A. S. |author9=Stensen |last10=Kawaler |first10=S. D. |last11=Telting |first11=J. H. | title=A compact system of small planets around a former red-giant star | journal=Nature | volume=480 | issue=7378 | date=21 December 2011 | issn=1476-4687 | doi=10.1038/nature10631 |pmid=22193103|pages=496–499|bibcode = 2011Natur.480..496C | s2cid=2213885 |display-authors=1}} but their existence are highly doubtful.{{citation | first=J. | last=Krzesinski | title=Planetary candidates around the pulsating sdB star KIC 5807616 considered doubtful | journal=Astronomy & Astrophysics | volume=581 | date=August 25, 2015 | pages=A7 | doi=10.1051/0004-6361/201526346 | bibcode=2015A&A...581A...7K | doi-access=free }}{{citation | first1=A. | last1=Blokesz | first2=J. | last2=Krzesinski | first3=L. | last3=Kedziora-Chudczer |

title=Analysis of putative exoplanetary signatures found in light curves of two sdBV stars observed by Kepler | journal=Astronomy & Astrophysics | volume=627 | date=4 July 2019 | pages=A86 | doi=10.1051/0004-6361/201835003 | bibcode=2019A&A...627A..86B | s2cid=182952925 | doi-access=free | arxiv=1906.03321 }}

Hottest (self-luminous)

|GQ Lupi b

|GQ Lupi

|2650 ± 100 K{{Cite journal |last1=Neuhäuser |first1=R. |last2=Mugrauer |first2=M. |last3=Seifahrt |first3=A. |last4=Schmidt |first4=T. O. B. |last5=Vogt |first5=N. |date=June 2008 |title=Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion |url=http://www.aanda.org/10.1051/0004-6361:20078493 |journal=Astronomy & Astrophysics |volume=484 |issue=1 |pages=281–291 |arxiv=0801.2287 |bibcode=2008A&A...484..281N |doi=10.1051/0004-6361:20078493 |issn=0004-6361}}
({{Val|2377|u=°C}})

| GQ Lupi b may be either a massive planet or a brown dwarf.

Coldest

| {{nowrap|OGLE-2005-BLG-390Lb }}

| {{nowrap|OGLE-2005-BLG-390L }}

| {{Convert|50|K|C}}{{Cite journal |last1=Beaulieu |first1=J. -P. |last2=Bennett |first2=D. P. |last3=Fouqué |first3=P. |last4=Williams |first4=A. |last5=Dominik |first5=M. |last6=Jørgensen |first6=U. G. |last7=Kubas |first7=D. |last8=Cassan |first8=A. |last9=Coutures |first9=C. |last10=Greenhill |first10=J. |last11=Hill |first11=K. |last12=Menzies |first12=J. |last13=Sackett |first13=P. D. |last14=Albrow |first14=M. |last15=Brillant |first15=S. |date=2006-01-01 |title=Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing |journal=Nature |volume=439 |issue=7075 |pages=437–440 |doi=10.1038/nature04441 |issn=0028-0836|doi-access=free |pmid=16437108 |arxiv=astro-ph/0601563 |bibcode=2006Natur.439..437B }}{{Efn|This is the calculated equilibrium temperature, assuming an albedo of 0.3}}

| {{nowrap|The disputed planet Proxima Centauri c}} may be cooler, at {{Convert|39|K|C}}.{{Cite journal |last1=Damasso |first1=Mario |last2=Del Sordo |first2=Fabio |last3=Anglada-Escudé |first3=Guillem |last4=Giacobbe |first4=Paolo |last5=Sozzetti |first5=Alessandro |last6=Morbidelli |first6=Alessandro |last7=Pojmanski |first7=Grzegorz |last8=Barbato |first8=Domenico |last9=Butler |first9=R. Paul |last10=Jones |first10=Hugh R. A. |last11=Hambsch |first11=Franz-Josef |last12=Jenkins |first12=James S. |last13=López-González |first13=María José |last14=Morales |first14=Nicolás |last15=Peña Rojas |first15=Pablo A. |date=2020-01-01 |title=A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU |journal=Science Advances |volume=6 |issue=3 |pages=eaax7467 |doi=10.1126/sciadv.aax7467|doi-access=free |pmid=31998838 |pmc=6962037 |bibcode=2020SciA....6.7467D }}

Fastest jetstream wind

| WASP-127b

| WASP-127

| 33 000 km/h
(9200 m/s){{Cite web |date=2024-10-01 |title=Detection of the resolved signatures of a supersonic equatorial jet and cool poles in a hot planet |url=https://www.eso.org/public/archives/releases/sciencepapers/eso2502/eso2502a.pdf |website=eso.org}}

Strongest magnetic field

| Tau Boötis b

| Tau Boötis

| {{val|117|38}} G{{Efn|Calculated assuming a ratio of 0.2% for the amount of total energy emitted in the Ca II K band.{{Cite journal|last1=Cauley|first1=P. Wilson|last2=Shkolnik|first2=Evgenya L.|last3=Llama|first3=Joe|last4=Lanza|first4=Antonino F.|date=Dec 2019|title=Magnetic field strengths of hot Jupiters from signals of star-planet interactions|journal=Nature Astronomy|volume=3|issue=12|pages=1128–1134|doi=10.1038/s41550-019-0840-x|arxiv=1907.09068|bibcode=2019NatAs...3.1128C|s2cid=198147426|issn=2397-3366}}}}

| For comparison, the field strength of Jupiter is 4.17 G.{{Cite journal |last1=Connerney |first1=J. E. P. |last2=Kotsiaros |first2=S. |last3=Oliversen |first3=R. J. |last4=Espley |first4=J. R. |last5=Joergensen |first5=J. L. |last6=Joergensen |first6=P. S. |last7=Merayo |first7=J. M. G. |last8=Herceg |first8=M. |last9=Bloxham |first9=J. |last10=Moore |first10=K. M. |last11=Bolton |first11=S. J. |last12=Levin |first12=S. M. |date=May 26, 2017 |title=A New Model of Jupiter's Magnetic Field From Juno's First Nine Orbits |url=http://orbit.dtu.dk/ws/files/147221632/Connerney_et_al_2018_Geophysical_Research_Letters.pdf |url-status=live |journal=Geophysical Research Letters |language=en |volume=45 |issue=6 |pages=2590–2596 |bibcode=2018GeoRL..45.2590C |doi=10.1002/2018GL077312 |archive-url=https://ghostarchive.org/archive/20221009/http://orbit.dtu.dk/ws/files/147221632/Connerney_et_al_2018_Geophysical_Research_Letters.pdf |archive-date=October 9, 2022 |doi-access=free}}

The magnetic field of SIMP J013656.5+093347 is

stronger at ~3200 G.{{Cite journal|last1=Kao|first1=Melodie M.|last2=Hallinan|first2=Gregg|last3=Pineda|first3=J. Sebastian|last4=Stevenson|first4=David|last5=Burgasser|first5=Adam|date=August 2018|title=The Strongest Magnetic Fields on the Coolest Brown Dwarfs|journal=Astrophysical Journal Supplement Series|language=en|volume=237|issue=2|pages=25|doi=10.3847/1538-4365/aac2d5|arxiv=1808.02485 |issn=0067-0049 |bibcode=2018ApJS..237...25K |doi-access=free }} As a free-floating object, it might not be considered as a planet.

Highest albedo

| LTT 9779 b

| LTT 9779

| 0.79 ± 0.15

| This is value for the western dayside region, with the overall albedo of dayside being 0.50 ± 0.07.{{Cite web |title=Highly Reflective White Clouds On The Western Dayside Of An Exo-Neptune |url=https://astrobiology.com/2025/01/highly-reflective-white-clouds-on-the-western-dayside-of-an-exo-neptune.html |access-date=2025-02-01 |website=astrobiology.com|date=28 January 2025 }}

For comparison, Earth is 0.3 and Venus is 0.76.

Lowest albedo

| {{nowrap|TrES-2b}}

| {{nowrap|GSC 03549-02811}}

| Geometric albedo {{nowrap|< 1%}}{{cite journal|author=David M. Kipping |display-authors=etal |title=Detection of visible light from the darkest world |journal=Monthly Notices of the Royal Astronomical Society |doi=10.1111/j.1745-3933.2011.01127.x |arxiv=1108.2297 |bibcode=2011MNRAS.417L..88K |volume=417 |issue=1 |pages=L88–L92 |year=2011 |doi-access=free |s2cid=119287494}}

| Best-fit model for albedo gives 0.04% (0.0004).

Youngest

|DH Tauri b

|DH Tauri

| {{val|0.7|0.3|0.2}} Myr{{Cite journal |last1=Xuan |first1=Jerry W. |last2=Hsu |first2=Chih-Chun |last3=Finnerty |first3=Luke |last4=Wang |first4=Jason |last5=Ruffio |first5=Jean-Baptiste |last6=Zhang |first6=Yapeng |last7=Knutson |first7=Heather A. |last8=Mawet |first8=Dimitri |last9=Mamajek |first9=Eric E. |last10=Inglis |first10=Julie |last11=Wallack |first11=Nicole L. |last12=Bryan |first12=Marta L. |last13=Blake |first13=Geoffrey A. |last14=Mollière |first14=Paul |last15=Hejazi |first15=Neda |date=2024-07-01 |title=Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of ~10–30 M Jup Companions |journal=The Astrophysical Journal |volume=970 |issue=1 |page=71 |arxiv=2405.13128 |bibcode=2024ApJ...970...71X |doi=10.3847/1538-4357/ad4796 |doi-access=free |issn=0004-637X}}

|The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.{{Cite encyclopedia |title=The Extrasolar Planet Encyclopaedia — Proplyd 133-353 |encyclopedia=Extrasolar Planets Encyclopaedia |url=https://exoplanet.eu/catalog/proplyd_133_353--4078/ |access-date=2019-03-30}} However, as a free-floating planet, it does not meet the IAU's working definition of a planet.

2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr, but fails the mass ratio criterion of the IAU working definition of an exoplanet; the mass ratio with the primary is larger than the L4/L5 limit of stability ≈ 1/25{{Cite journal |last1=Lecavelier des Etangs |first1=A. |last2=Lissauer |first2=Jack J. |date=2022-06-01 |title=The IAU working definition of an exoplanet |url=https://linkinghub.elsevier.com/retrieve/pii/S138764732200001X |journal=New Astronomy Reviews |language=en |volume=94 |pages=101641 |arxiv=2203.09520 |bibcode=2022NewAR..9401641L |doi=10.1016/j.newar.2022.101641}} and the companion is 'more likely to have been produced by cloud core fragmentation' (similar to a star).{{Cite journal |last1=Todorov |first1=K. |last2=Luhman |first2=K. L. |last3=McLeod |first3=K. K. |date=2010-05-01 |title=Discovery of a Planetary-Mass Companion to a Brown Dwarf in Taurus |url=https://iopscience.iop.org/article/10.1088/2041-8205/714/1/L84 |journal=The Astrophysical Journal |volume=714 |issue=1 |pages=L84–L88 |arxiv=1004.0539 |bibcode=2010ApJ...714L..84T |doi=10.1088/2041-8205/714/1/L84 |issn=2041-8205}}

Two planetary candidates proposed to orbit IRS 63 are at ≲0.5 Myr.{{cite journal |arxiv=2010.03657 |doi=10.1038/s41586-020-2779-6 |title=Four annular structures in a protostellar disk less than 500,000 years old |date=2020 |last1=Segura-Cox |first1=Dominique M. |last2=Schmiedeke |first2=Anika |last3=Pineda |first3=Jaime E. |last4=Stephens |first4=Ian W. |last5=Fernández-López |first5=Manuel |last6=Looney |first6=Leslie W. |last7=Caselli |first7=Paola |last8=Li |first8=Zhi-Yun |last9=Mundy |first9=Lee G. |last10=Kwon |first10=Woojin |last11=Harris |first11=Robert J. |journal=Nature |volume=586 |issue=7828 |pages=228–231 |pmid=33028998 }}

IRAS 04125+2902 b is the youngest transiting planet at an age of ~3 Myr.{{Cite journal |last1=Barber |first1=Madyson G. |last2=Mann |first2=Andrew W. |last3=Vanderburg |first3=Andrew |last4=Krolikowski |first4=Daniel |last5=Kraus |first5=Adam |last6=Ansdell |first6=Megan |last7=Pearce |first7=Logan |last8=Mace |first8=Gregory N. |last9=Andrews |first9=Sean M. |last10=Boyle |first10=Andrew W. |last11=Collins |first11=Karen A. |last12=De Furio |first12=Matthew |last13=Dragomir |first13=Diana |last14=Espaillat |first14=Catherine |last15=Feinstein |first15=Adina D. |date=November 2024 |title=A giant planet transiting a 3-Myr protostar with a misaligned disk |url=https://www.nature.com/articles/s41586-024-08123-3 |journal=Nature |language=en |volume=635 |issue=8039 |pages=574–577 |doi=10.1038/s41586-024-08123-3 |pmid=39567788 |arxiv=2411.18683 |bibcode=2024Natur.635..574B |issn=1476-4687}}

CI Tauri c would be the youngest radial velocity planet at an age of 2–3 Myr, if confirmed.{{Cite journal |last1=Manick |first1=R. |last2=Sousa |first2=A. P. |last3=Bouvier |first3=J. |last4=Almenara |first4=J. M. |last5=Rebull |first5=L. |last6=Bayo |first6=A. |last7=Carmona |first7=A. |last8=Martioli |first8=E. |last9=Venuti |first9=L. |last10=Pantolmos |first10=G. |last11=Kóspál |first11=á. |last12=Zanni |first12=C. |last13=Bonfils |first13=X. |last14=Moutou |first14=C. |last15=Delfosse |first15=X. |date=June 2024 |title=Long-period modulation of the classical T Tauri star CI Tau: Evidence for an eccentric close-in massive planet at 0.17 au |url=https://www.aanda.org/10.1051/0004-6361/202348258 |journal=Astronomy & Astrophysics |volume=686 |pages=A249 |arxiv=2403.03706 |bibcode=2024A&A...686A.249M |doi=10.1051/0004-6361/202348258 |issn=0004-6361}}{{efn|1=Most sources like the NASA Exoplanet Archive and exoplanet.eu already accept it as confirmed.{{cite web |url=https://exoplanetarchive.ipac.caltech.edu/overview/CI%20Tau |title=CI Tau |website=NASA Exoplanet Archive |access-date=29 March 2024}}{{cite EPE|title=CI Tau c|id=10725}}}}

Oldest

| TOI-157 b

| TOI-157

| {{Val|12.82|0.73|1.40|ul=}} Gyr{{Cite journal |last1=Nielsen |first1=L. D. |last2=Brahm |first2=R. |last3=Bouchy |first3=F. |last4=Espinoza |first4=N. |last5=Turner |first5=O. |last6=Rappaport |first6=S. |last7=Pearce |first7=L. |last8=Ricker |first8=G. |last9=Vanderspek |first9=R. |last10=Latham |first10=D. W. |last11=Seager |first11=S. |last12=Winn |first12=J. N. |last13=Jenkins |first13=J. M. |last14=Acton |first14=J. S. |last15=Bakos |first15=G. |date=July 2020 |title=Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b |url=https://www.aanda.org/10.1051/0004-6361/202037941 |journal=Astronomy & Astrophysics |volume=639 |pages=A76 |arxiv=2003.05932 |bibcode=2020A&A...639A..76N |doi=10.1051/0004-6361/202037941 |issn=0004-6361}}

| The currently accepted age of the universe is around 13.8 billion years. Could alternatively be PSR B1620-26 b with 11.2–12.7 Gyr.{{Cite journal |last1=Lacki |first1=Brian C. |last2=Brzycki |first2=Bryan |last3=Croft |first3=Steve |last4=Czech |first4=Daniel |last5=DeBoer |first5=David |last6=DeMarines |first6=Julia |last7=Gajjar |first7=Vishal |last8=Isaacson |first8=Howard |last9=Lebofsky |first9=Matt |last10=MacMahon |first10=David H. E. |last11=Price |first11=Danny C. |last12=Sheikh |first12=Sofia Z. |last13=Siemion |first13=Andrew P. V. |last14=Drew |first14=Jamie |last15=Worden |first15=S. Pete |date=2021-12-01 |title=One of Everything: The Breakthrough Listen Exotica Catalog |journal=The Astrophysical Journal Supplement Series |volume=257 |issue=2 |pages=42 |arxiv=2006.11304 |bibcode=2021ApJS..257...42L |doi=10.3847/1538-4365/ac168a |issn=0067-0049 |doi-access=free}}

Two disproven planets had been thought to orbit the star HIP 11952,{{Cite journal|bibcode = 2014A&A...562A.129J|title = No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044|last1 = Jones|first1 = M. I.|last2 = Jenkins|first2 = J. S.|journal = Astronomy and Astrophysics|year = 2014|volume = 562|pages = A129|doi = 10.1051/0004-6361/201322132|arxiv = 1401.0517|s2cid = 55365608}} whose age is {{Val|12.8|2.6}} Gyr.{{cite encyclopedia | url=http://exoplanet.eu/star.php?st=HIP+11952 | archive-url=https://web.archive.org/web/20120505093906/http://exoplanet.eu/star.php?st=HIP+11952 | url-status=dead | archive-date=May 5, 2012 | title=Notes for Star HIP 11952 | date=23 March 2012 | access-date=March 29, 2012 | encyclopedia=Extrasolar Planets Encyclopaedia | author=Schneider, Jean}}

The star HE 1523-0901 might be older at 13.2 Gyr

{{cite journal

|last1= Frebel|first1=A.

|display-authors=etal

|date=2007

|journal=The Astrophysical Journal |volume=660 |issue=2 |page=L117

|title=Discovery of HE 1523–0901, a Strongly r-Process-enhanced Metal-poor Star with Detected Uranium

|arxiv=astro-ph/0703414

|bibcode=2007ApJ...660L.117F

|doi=10.1086/518122

|s2cid=17533424

}} and has a candidate planet or brown dwarf.{{citation|arxiv=1509.05344|year=2015|title=The role of binaries in the enrichment of the early Galactic halo. I. r-process-enhanced metal-poor stars|doi=10.1051/0004-6361/201526812 |last1=Hansen |first1=T. T. |last2=Andersen |first2=J. |last3=Nordström |first3=B. |last4=Beers |first4=T. C. |last5=Yoon |first5=J. |last6=Buchhave |first6=L. A. |journal=Astronomy & Astrophysics |volume=583 |pages=A49 |bibcode=2015A&A...583A..49H }}

Orbital characteristics

class="wikitable sticky-header" style="text-align:left;"
style="background:#efefef;"\| Title ! style="background:#efefef;"\| Planet ! style="background:#efefef;"\| Star ! style="background:#efefef;"\| Data ! style="background:#efefef;"\| Notes
Longest orbital period (Longest year) \| Gliese 900 b (CW2335+0142) \| Gliese 900 \| 1.27 million years{{Cite web \|title=GJ 900 b - NASA Science \|url=https://science.nasa.gov/exoplanet-catalog/gj-900-b/ \|access-date=2024-06-20 \|website=science.nasa.gov \|date=31 May 2024 \|language=en-US}}{{Efn\|name=fn5\|Assuming a circular orbit and using the Kepler's Third law}} \| COCONUTS-2b previously held this record at 1,100,000 years.{{Efn\|name=fn5}}
Shortest orbital period (Shortest year) \| GALEX 0718+3731 b \| GALEX 0718+3731 \| {{nowrap\|0.187 h}} (11.2 minutes) \| KOI 1843.03 has the shortest orbit around a main-sequence star (an M dwarf) at 4.25 hours.{{cite web \|title=Kepler-974 \|url=https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-974 \|website=NASA Exoplanet Archive \|publisher=Caltech \|access-date=14 March 2025}}
Largest orbital separation \|Gliese 900 b (CW2335+0142) \|Gliese 900 \|12 000 AU \|UCAC4 328-061594 b has an even larger orbital separation (19 000 AU), although its mass (21 `M`_J) is higher than the deuterium burning limit (13 `M`_J). Another candidate around BD+29 5007 has an even larger orbit of about 22 100 AU. There is no consensus about its age and the resulting mass, and it could be a field brown dwarf. The companion of ASASSN-21js has an orbit of about 13 000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass.{{Cite journal \|last1=Pramono \|first1=T. H. \|last2=Kenworthy \|first2=M. A. \|last3=Boekel \|first3=R. van \|date=2024-08-01 \|title=ASASSN-21js: A multi-year transit of a ringed disc \|url=https://www.aanda.org/articles/aa/full_html/2024/08/aa50288-24/aa50288-24.html \|journal=Astronomy & Astrophysics \|language=en \|volume=688 \|pages=L11 \|doi=10.1051/0004-6361/202450288 \|arxiv=2408.06744 \|bibcode=2024A&A...688L..11P \|issn=0004-6361}}
Smallest orbital separation (smallest semi-major axis) \| GALEX 0718+3731 b \| GALEX 0718+3731 \| 0.000834 AU \| TOI-6324 b has the smallest orbital separation from a main-sequence star (an M dwarf) at ~0.0043 AU.{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — TOI-6324 b. \|url=https://exoplanet.eu/catalog/toi_6324_b--10860/}}
Most eccentric orbit \| HD 20782 b \| HD 20782 \| 0.950 \| Could alternatively be HD 28254 b with an eccentricity at {{val\|0.95\|0.03\|0.04}}. The possible planets HD 205577 b and SGR 1806-20 b have even higher eccentricities at {{val\|0.972\|0.08\|0.002}} and 0.994, respectively.{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — HD 205577 b. \|url=https://exoplanet.eu/catalog/hd_205577_b--7219/}}{{Citation \|last1=Kurban \|first1=Abdusattar \|title=Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet \|date=2024-03-20 \|journal=Astronomy & Astrophysics \|volume=686 \|pages=A87 \|arxiv=2403.13333 \|bibcode=2024A&A...686A..87K \|doi=10.1051/0004-6361/202347828 \|last2=Zhou \|first2=Xia \|last3=Wang \|first3=Na \|last4=Huang \|first4=Yong-Feng \|last5=Wang \|first5=Yu-Bin \|last6=Nurmamat \|first6=Nurimangul}} The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.{{Cite encyclopedia \|title=The Extrasolar Planet Encyclopaedia — VB 10 b \|encyclopedia=Extrasolar Planets Encyclopaedia \|url=https://exoplanet.eu/catalog/vb_10_b--550/ \|access-date=2020-02-12}}
Highest orbital inclination \|HD 204313 e \|HD 204313 \|{{Val\|176.092\|0.963\|2.122\|ul=deg}} \|{{Cite journal \|last1=Feng \|first1=Fabo \|last2=Butler \|first2=R. Paul \|last3=Vogt \|first3=Steven S. \|last4=Clement \| first4=Matthew S. \|last5=Tinney \|first5=C. G. \|last6=Cui \|first6=Kaiming \|last7=Aizawa \|first7=Masataka \|last8=Jones \|first8=Hugh R. A. \|last9=Bailey \|first9=J. \|last10=Burt \|first10=Jennifer \|last11=Carter \|first11=B. D. \|last12=Crane \|first12=Jeffrey D. \|last13=Flammini Dotti \|first13=Francesco \|last14=Holden \|first14=Bradford \|last15=Ma \|first15=Bo \|date=2022-09-01 \|title=3D Selection of 167 Substellar Companions to Nearby Stars \|journal=The Astrophysical Journal Supplement Series \|volume=262 \|issue=1 \|pages=21 \|doi=10.3847/1538-4365/ac7e57 \|doi-access=free \|arxiv=2208.12720 \|bibcode=2022ApJS..262...21F \|issn=0067-0049}}
Lowest orbital inclination \|HD 331093 b \|HD 331093 \|{{val\|0.3704\|p=>\|u=deg}} \|{{Cite journal \|last1=Dalal \|first1=S. \|last2=Kiefer \|first2=F. \|last3=Hébrard \|first3=G. \|last4=Sahlmann \|first4=J. \|last5=Sousa \|first5=S. G. \|last6=Forveille \|first6=T. \|last7=Delfosse \|first7=X. \|last8=Arnold \|first8=L. \|last9=Astudillo-Defru \|first9=N. \|last10=Bonfils \|first10=X. \|last11=Boisse \|first11=I. \|last12=Bouchy \|first12=F. \|last13=Bourrier \|first13=V. \|last14=Brugger \|first14=B. \|last15=Cortés-Zuleta \|first15=P. \|date=2021-07-01 \|title=The SOPHIE search for northern extrasolar planets. XVII. A wealth of new objects: Six cool Jupiters, three brown dwarfs, and 16 low-mass binary stars \|url=https://ui.adsabs.harvard.edu/abs/2021A&A...651A..11D \|journal=Astronomy and Astrophysics \|volume=651 \|pages=A11 \|doi=10.1051/0004-6361/202140712 \|arxiv=2105.09741 \|bibcode=2021A&A...651A..11D \|issn=0004-6361}} HD 43197 c has the lowest orbital inclination that is not a lower limit, of {{val\|11.42\|5.388\|3.07\|u=deg}}.{{Cite web \|title=Planetary Systems \|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PS \|access-date=2024-01-15 \|website=exoplanetarchive.ipac.caltech.edu}}
Largest semi-amplitude \| WASP-18b \| WASP-18 \| {{val\|1814\|23\|24}} m/s \| {{cite journal \|last1=Cortés-Zuleta \|first1=Pía \|last2=Rojo \|first2=Patricio \|display-authors=etal \|date=April 2020 \|title=TraMoS. V. Updated ephemeris and multi-epoch monitoring of the hot Jupiters WASP-18Ab, WASP-19b, and WASP-77Ab \|journal=Astronomy & Astrophysics \|volume=636 \|issue= \|pages=A98 \|doi=10.1051/0004-6361/201936279 \|arxiv=2001.11112 \|bibcode=2020A&A...636A..98C \|s2cid=241596186 }} The planetary-mass objects CoRoT-3b, GPX-1 b and KELT-1Ab have larger semi-amplitudes at {{val\|2173\|25}} m/s,{{cite web \|year=2025 \|website= exoplanetarchive.ipac.caltech.edu \|title= CoRoT-3 Overview \|url= https://exoplanetarchive.ipac.caltech.edu/overview/CoRoT-3}} {{val\|2310\|180}} m/s{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — GPX-1 b. \|url=https://exoplanet.eu/catalog/gpx_1_b--7504/}} and {{val\|4239\|52}} m/s,{{Cite journal \|last1=Siverd \|first1=Robert J. \|last2=Beatty \|first2=Thomas G. \|last3=Pepper \|first3=Joshua \|last4=Eastman \|first4=Jason D. \|last5=Collins \|first5=Karen \|last6=Bieryla \|first6=Allyson \|last7=Latham \|first7=David W. \|last8=Buchhave \|first8=Lars A. \|last9=Jensen \|first9=Eric L. N. \|last10=Crepp \|first10=Justin R. \|last11=Street \|first11=Rachel \|last12=Stassun \|first12=Keivan G. \|last13=Scott Gaudi \|first13=B. \|last14=Berlind \|first14=Perry \|last15=Calkins \|first15=Michael L. \|date=2012-12-04 \|title=KELT-1b: A STRONGLY IRRADIATED, HIGHLY INFLATED, SHORT PERIOD, 27 JUPITER-MASS COMPANION TRANSITING A MID-F STAR \|journal=The Astrophysical Journal \|volume=761 \|issue=2 \|pages=123 \|doi=10.1088/0004-637x/761/2/123 \|issn=0004-637X\|arxiv=1206.1635 }} respectively; however they are likely brown dwarfs rather than planets.{{Cite journal \| title=Transiting exoplanets from the CoRoT space mission. VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert \| url=https://www.aanda.org/articles/aa/full/2008/45/aa10625-08/aa10625-08.html \|last1=Deleuil \| first1=M. \| last2=Deeg \| first2=H. J. \| last3=Alonso \| first3=R. \| last4=Bouchy \| first4=F. \| last5=Rouan \| first5=D. \| last6=Auvergne \| first6=M. \| last7=Baglin \| first7=A. \| last8=Aigrain \| first8=S. \| last9=Almenara \| first9=J. M. \| last10=Barbieri \| first10=M. \| last11=Barge \| first11=P. \| last12=Bruntt \| first12=H. \| last13=Bordé \| first13=P. \| last14=Collier Cameron \| first14=A. \| last15=Csizmadia \| first15=S.. \| last16=De La Reza \| first16=R. \| last17=Dvorak \| first17=R. \| last18=Erikson \| first18=A. \| last19=Fridlund \| first19=M. \| last20=Gandolfi \| first20=D. \| last21=Gillon \| first21=M. \| last22=Guenther \| first22=E. \| last23=Guillot \| first23=T. \| last24=Hatzes \| first24=A. \| last25=Hébrard \| first25=G. \| last26=Jorda \| first26=L. \| last27=Lammer \| first28=A. \| first29=A. \| last30=Loeillet \| first30=B. \| last28=Léger \| last29=Llebaria \| first27=H. \|display-authors=1 \|journal=Astronomy and Astrophysics \|volume=491 \| issue=3 \| pages=889–897 \| year=2008 \| arxiv=0810.0919 \| bibcode=2008A&A...491..889D \| doi=10.1051/0004-6361:200810625 \| s2cid=8944836 }}
Smallest semi-amplitude \| Barnard's Star e \| Barnard's Star \| {{val\|0.221\|0.038}} m/s \|
Largest orbit around a single star \| COCONUTS-2b \| L 34-26 \| 7506 AU \| Next largest are 2MASS J2126–8140 with 6900 AU and HD 106906 b{{cite journal \|title=A Near-coplanar Stellar Flyby of the Planet Host Star HD 106906 \|journal=The Astronomical Journal \|first1=Robert J. \|last1=De Rosa \|first2=Paul \|last2=Kalas \|volume=157 \|issue=3 \|at=125 \|date=February 2019 \|doi=10.3847/1538-3881/ab0109 \|bibcode=2019AJ....157..125D \|arxiv=1902.10220\|s2cid=119191779 \|doi-access=free }} with ~738 AU. UCAC4 328-061594 b has a significantly larger orbital separation (about 19,000 AU), although its mass ({{Jupiter mass\|21\|link=y}}){{Cite journal \|last1=Rothermich \|first1=Austin \|last2=Faherty \|first2=Jacqueline K. \|last3=Bardalez-Gagliuffi \|first3=Daniella \|last4=Schneider \|first4=Adam C. \|last5=Kirkpatrick \|first5=J. Davy \|last6=Meisner \|first6=Aaron M. \|last7=Burgasser \|first7=Adam J. \|last8=Kuchner \|first8=Marc \|last9=Allers \|first9=Katelyn \|last10=Gagné \|first10=Jonathan \|last11=Caselden \|first11=Dan \|last12=Calamari \|first12=Emily \|last13=Popinchalk \|first13=Mark \|last14=Suárez \|first14=Genaro \|last15=Gerasimov \|first15=Roman \|date=2024-06-01 \|title=89 New Ultracool Dwarf Comoving Companions Identified with the Backyard Worlds: Planet 9 Citizen Science Project \|journal=The Astronomical Journal \|volume=167 \|issue=6 \|pages=253 \|arxiv=2403.04592 \|bibcode=2024AJ....167..253R \|doi=10.3847/1538-3881/ad324e \|issn=0004-6256 \|doi-access=free}} is higher than the deuterium burning limit ({{Jupiter mass\|13\|link=y}}).
Smallest orbit around binary star \| {{nowrap\|Kepler-47b}} \| {{nowrap\|Kepler-47}} \| {{val\|0.2877\|0.0014\|0.0011\|u=AU}} \|{{cite journal \| journal= Science \|title= Kepler-47: A Transiting Circumbinary Multi-Planet System \|date= 2012\|author1= Orosz, J. \|author2= Welsh, W. \|author3= Carter, J.\|author4= Fabrycky, D. \|author5= Cochran, W. \| display-authors= etal \| doi= 10.1126/science.1228380 \| volume= 337 \| issue= 6101 \| pages= 1511–4 \| pmid= 22933522 \|bibcode= 2012Sci...337.1511O \|arxiv= 1208.5489 \|s2cid=44970411}} Kepler-1521 b has a smaller orbit with semi-major axis at {{val\|0.2347\|0.0011\|u=AU}}. The planet might be circumbinary, as the binarity of host star is suggested but not confirmed.{{Cite arXiv \|last1=Kamai \|first1=Ilay \|last2=Perets \|first2=Hagai B. \|title=Too fast to be single: Tidal evolution and photometric identification of stellar and planetary companions \|date=March 2025 \|class=astro-ph.SR \|eprint=2503.03839 }}
Smallest ratio of semi-major axis of binary star orbit to a planet orbiting one of the stars (S-type planet) \| Nu Octantis Ab \| Nu Octantis \| 2.06 \| {{cite journal \|author1=Ramm, D. J. \|display-authors=etal \|date=2016 \|title=The conjectured S-type retrograde planet in ν Octantis: more evidence including four years of iodine-cell radial velocities \|journal=Monthly Notices of the Royal Astronomical Society \|volume=460 \|issue=4 \|pages=3706–3719 \|arxiv=1605.06720 \|bibcode=2016MNRAS.460.3706R \|doi=10.1093/mnras/stw1106 \|doi-access=free}}
Largest orbit around binary star \|SR 12 c \|SR 12 \|≈1100 AU{{Cite journal \|last1=Kuzuhara \|first1=M. \|last2=Tamura \|first2=M. \|last3=Ishii \|first3=M. \|last4=Kudo \|first4=T. \|last5=Nishiyama \|first5=S. \|last6=Kandori \|first6=R. \|date=2011-04-01 \|title=The Widest-Separation Substellar Companion Candidate to a Binary T Tauri Star \|url=https://iopscience.iop.org/article/10.1088/0004-6256/141/4/119 \|journal=The Astronomical Journal \|volume=141 \|issue=4 \|pages=119 \|bibcode=2011AJ....141..119K \|doi=10.1088/0004-6256/141/4/119 \|issn=0004-6256}} \| SR 12 c has a mass of {{val\|0.013\|0.007\|ul=Solar mass}}. {{nowrap\|DT Virginis c}}, also known as Ross 458 c, at a projected separation of ≈1200 AU, with several mass estimates below the deuterium burning limit, has a latest mass determination of {{val\|27\|4\|ul=}} {{Jupiter mass}}.{{Cite journal \|last1=Gaarn \|first1=Josefine \|last2=Burningham \|first2=Ben \|last3=Faherty \|first3=Jacqueline K \|last4=Visscher \|first4=Channon \|last5=Marley \|first5=Mark S \|last6=Gonzales \|first6=Eileen C \|last7=Calamari \|first7=Emily \|last8=Bardalez Gagliuffi \|first8=Daniella \|last9=Lupu \|first9=Roxana \|last10=Freedman \|first10=Richard \|date=2023-03-31 \|title=The puzzle of the formation of T8 dwarf Ross 458c \|url=https://academic.oup.com/mnras/article/521/4/5761/7078574 \|journal=Monthly Notices of the Royal Astronomical Society \|language=en \|volume=521 \|issue=4 \|pages=5761–5775 \|arxiv=2303.16863 \|bibcode=2023MNRAS.521.5761G \|doi=10.1093/mnras/stad753 \|doi-access=free \|issn=0035-8711}} The binary 2MASS J0249-0557 AB has a planetary mass companion less massive than 13 M_J at a larger separation of 1950 ± 200 AU, although this companion might have formed as a brown dwarf based on the mass ratio to the primary.{{Cite journal \|last1=Dupuy \|first1=Trent J. \|last2=Liu \|first2=Michael C. \|last3=Allers \|first3=Katelyn N. \|last4=Biller \|first4=Beth A. \|last5=Kratter \|first5=Kaitlin M. \|last6=Mann \|first6=Andrew W. \|last7=Shkolnik \|first7=Evgenya L. \|last8=Kraus \|first8=Adam L. \|last9=Best \|first9=William M. J.\|date=2018-08-01 \|title=The Hawaii Infrared Parallax Program. III. 2MASS J0249-0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group \|journal=The Astronomical Journal \|volume=156 \|issue=2 \|pages=57 \|arxiv=1807.05235 \|bibcode=2018AJ....156...57D \|doi=10.3847/1538-3881/aacbc2 \|doi-access=free \|issn=0004-6256}}
Largest orbit around a single star in a multiple star system \| DH Tauri b \| DH Tauri \| ≈330 AU{{Cite journal \|last1=Itoh \|first1=Yoichi \|last2=Hayashi \|first2=Masahiko \|last3=Tamura \|first3=Motohide \|last4=Tsuji \|first4=Takashi \|last5=Oasa \|first5=Yumiko \|last6=Fukagawa \|first6=Misato \|last7=Hayashi \|first7=Saeko S. \|last8=Naoi \|first8=Takahiro \|last9=Ishii \|first9=Miki \|last10=Mayama \|first10=Satoshi \|last11=Morino \|first11=Jun-ichi \|last12=Yamashita \|first12=Takuya \|last13=Pyo \|first13=Tae-Soo \|last14=Nishikawa \|first14=Takayuki \|last15=Usuda \|first15=Tomonori \|date=2005-02-20 \|title=A Young Brown Dwarf Companion to DH Tauri \|url=https://iopscience.iop.org/article/10.1086/427086 \|journal=The Astrophysical Journal \|language=en \|volume=620 \|issue=2 \|pages=984–993 \|arxiv=astro-ph/0411177 \|bibcode=2005ApJ...620..984I \|doi=10.1086/427086 \|issn=0004-637X}} \|
Largest separation between binary stars with a circumbinary planet \| SR 12 c \| SR 12 \| ≈26 AU \| SR 12 c has a mass of {{val\|0.013\|0.007\|ul=Solar mass}} at a projected separation of ≈1100 AU. FW Tauri b orbits at a projected separation of {{val\|330\|30\|ul=AU}} around a ≈11 AU separated binary.{{Cite journal\|last1=Kraus\|first1=Adam\|last2=J. Ireland\|first2=Michael\|last3=A. Cieza\|first3=Lucas\|last4=Hinkley\|first4=Sasha\|last5=J. Dupuy\|first5=Trent\|last6=P. Bowler\|first6=Brendan\|last7=C. Liu\|first7=Michael \|date=2014-01-02\|title=Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B\|journal= The Astrophysical Journal\|volume=781\|issue=1\|page=1311\|arxiv=1311.7664\|doi=10.1088/0004-637X/781/1/20\|bibcode=2014ApJ...781...20K\|s2cid=41086512}} It was shown to be likely a {{val\|0.1	ul=Solar mass}} star surrounded by a protoplanetary disk rather than a planetary-mass companion.{{Cite journal \|last1=Mora \|first1=Ariel \|last2=Wu \|first2=Ya-Lin \|last3=Bowler \|first3=Brendan P. \|last4=Sheehan \|first4=Patrick \|date=2020-01-01 \|title=Measuring the Mass of the Faint Companion to FW Tau with ALMA \|journal=Research Notes of the AAS \|volume=4 \|issue=1 \|pages=9 \|doi=10.3847/2515-5172/ab6852 \|doi-access=free \|bibcode=2020RNAAS...4....9M \|issn=2515-5172}}
Largest orbit around three stars \| Gliese 900 b (CW2335+0142) \| Gliese 900 \|12 000 AU \|
Closest orbit between stars with a planet orbiting one of the stars (S-type planet) \| {{nowrap\|DMPP-3 Ab}} \| HD 42936 \|1.139 AU{{cite journal \|arxiv=1912.10793 \|doi=10.1038/s41550-019-0972-z \|title=An ablating 2.6-M_🜨 planet in an eccentric binary from the Dispersed Matter Planet Project \|journal=Nature Astronomy \|year=2019 \|last1=Barnes \|first1=John R. \|last2=Haswell \|first2=Carole A. \|last3=Staab \|first3=Daniel \|last4=Anglada-Escudé \|first4=Guillem \|last5=Fossati \|first5=Luca \|last6=Doherty \|first6=James P. J. \|last7=Cooper \|first7=Joseph \|last8=Jenkins \|first8=James S. \|last9=Díaz \|first9=Matías R. \|last10=Soto \|first10=Maritza G. \|last11=Peña Rojas \|first11=Pablo A. \|volume=4 \|issue=4 \|pages=419–426 \|s2cid=209444780}}{{Cite web \|date=March 2024 \|title=Multiplicity of stars with planets in the solar neighbourhood \|url=https://www.aanda.org/articles/aa/pdf/forth/aa50048-24.pdf \|website=aanda.org}} \| DMPP-3 Ab's semi-major axis is around 0.067 AU.
Closest orbit between stars with planets orbiting both the stars \| HD 133131 Ab, c and HD 133131 Bb \| HD 133131 A and HD 133131 B \|360 AU \|The outer planet of HD 133131 A has a semi-major axis of 4.79 AU while the only planet known of HD 133131 B has a semi-major axis of 6.40 AU.{{cite journal \|bibcode=2016AJ....152..167T\|doi=10.3847/0004-6256/152/6/167\|arxiv=1608.06216\|title=The Magellan PFS Planet Search Program: Radial Velocity and Stellar Abundance Analyses of the 360 AU, Metal-Poor Binary "Twins" HD 133131A & B\|journal=The Astronomical Journal\|volume=152\|issue=6\|pages=167\|year=2016\|last1=Teske\|first1=Johanna K\|last2=Shectman\|first2=Stephen A\|last3=Vogt\|first3=Steve S\|last4=Díaz\|first4=Matías \|last5=Butler \|first5=R. Paul \|last6=Crane \|first6=Jeffrey D \|last7=Thompson \|first7=Ian B \|last8=Arriagada \|first8=Pamela \|s2cid=118852162 \|doi-access=free }}
Smallest semi-major axis ratio between consecutive planets \| Kepler-36b and Kepler-36c \| Kepler-36 \| 1.11 \| Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively; hence the planet c is 1.11 times further from star than b. 2MASS J1657-5343 b and 2MASS J1657-5343 c have semi-major axes of 165 AU and 180 AU, resulting in the planet c being ~1.09 times further from star than b.{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — 2MASS J1657-5343 b. \|url=https://voparis-exoplanet-new.obspm.fr/catalog/2mass_j1657_5343_b--9993/}}{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — 2MASS J1657-5343 c. \|url=https://voparis-exoplanet-new.obspm.fr/catalog/2mass_j1657_5343_c--9994/}} Despite being listed in EPE as planets, these companions are most likely brown dwarfs based on the mass. There have been unconfirmed detections of co-orbital pairs of exoplanet, each of which has a semi-major axis ratio of almost 1.
Largest stellar radius \| HD 220074 b \| HD 220074 \| {{val\|59.60\|5.85\|6.31\|ul=Solar radius}}{{Cite Gaia DR2\|2014988549785194752}} \| Other stars, such as HD 18438, Mirach and Delta Virginis are larger, but their substellar companions are more massive than the deuterium burning limit at about {{Jupiter mass\|13\|link=y}}, and thus might be brown dwarfs rather than exoplanets. {{Nowrap\|Candidate planets were reported around the}} red giants V Camelopardalis ({{val\|716\|185\|u=Solar radius}}),{{Cite journal \|last1=van Belle \|first1=G. T. \|last2=Thompson \|first2=R. R. \|last3=Creech-Eakman \|first3=M. J. \|date=September 2002 \|title=Angular Size Measurements Of Mira Variable Stars At 2.2 Microns. II \|arxiv=astro-ph/0210167 \|journal=The Astronomical Journal \|volume=124 \|issue=3 \|pages=1706–1715 \|doi=10.1086/342282\|bibcode=2002AJ....124.1706V }} R Fornacis ({{Solar radius calculator\|8\|0.68\|type=AD\|unit=y}}{{Efn\|1=Determined using known angular diameter and distance. 0.008 milliarcseconds * 680 pc = diameter of 5.44 au.}}),{{Cite journal \|last1=Paladini \|first1=C. \|last2=Sacuto \|first2=S. \|last3=Klotz \|first3=D. \|last4=Ohnaka \|first4=K. \|last5=Wittkowski \|first5=M. \|last6=Nowotny \|first6=W. \|last7=Jorissen \|first7=A. \|last8=Hron \|first8=J. \|date=2012-08-01 \|title=Detection of an asymmetry in the envelope of the carbon Mira R Fornacis using VLTI/MIDI \|url=https://www.aanda.org/articles/aa/abs/2012/08/aa19831-12/aa19831-12.html \|journal=Astronomy & Astrophysics \|language=en \|volume=544 \|pages=L5 \|doi=10.1051/0004-6361/201219831 \|issn=0004-6361\|arxiv=1207.3910 \|bibcode=2012A&A...544L...5P }}{{Cite EPE\|name=R For b\|access-date=July 19, 2024\|id=10018}} V Hydrae ({{solar radius\|430}}),{{Cite journal \|last1=Salas \|first1=Jesus M. \|last2=Naoz \|first2=Smadar \|last3=Morris \|first3=Mark R. \|last4=Stephan \|first4=Alexander P. \|date=2019-08-11 \|title=Unseen companions of V Hya inferred from periodic ejections \|arxiv=1902.08206 \|journal=Monthly Notices of the Royal Astronomical Society \|volume=487 \|issue=3 \|pages=3029–3036 \|doi=10.1093/mnras/stz1515 \|doi-access=free \|issn=0035-8711}} R Leonis ({{Solar radius\|320-350}}){{Cite journal \| arxiv=0809.0359 \| author=Wiesemeyer \| display-authors=etal \| title=Precessing planetary magnetospheres in SiO stars?. First detection of quasi-periodic polarization fluctuations in R Leonis and V Camelopardalis\| journal=Astronomy and Astrophysics \| volume=498 \| issue=3 \| pages=801–810 \| date=2009 \| bibcode=2009A&A...498..801W\|doi = 10.1051/0004-6361/200811242 \| s2cid=14531031 }}{{Cite journal \|arxiv=astro-ph/0411133 \|author=Fedele \|display-authors=etal \|title=The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI \|journal=Astronomy & Astrophysics \| volume=431 \|issue=3 \| pages=1019–1026 \| date=2005 \| bibcode=2005A&A...431.1019F\|doi = 10.1051/0004-6361:20042013 \| s2cid=15500217}} and L2 Puppis ({{val\|123\|14\|u=Solar radius}}). The stars R126 and R66 in the Large Magellanic Cloud have radii of {{Solar radius\|78}} and {{Solar radius\|131}}{{Cite journal \| last1 = Kastner \| first1 = J. H. \| last2 = Buchanan \| first2 = C. L. \| last3 = Sargent \| first3 = B. \| last4 = Forrest \| first4 = W. J. \| title = SpitzerSpectroscopy of Dusty Disks around B\e] Hypergiants in the Large Magellanic Cloud \| doi = 10.1086/500804 \| journal = The Astrophysical Journal \| volume = 638 \| pages = L29–L32 \| year = 2006 \| issue = 1 \|bibcode = 2006ApJ...638L..29K \| doi-access = free }} and have dust discs but no planets have been detected yet.
Smallest stellar radius \| PSR J1211-0633 b \| PSR J1211-0633 \| {{cvt\|0.0000143\|solar radius\|km\|abbr=on}}{{cite EPE\|name=PSR J1211-0633 b\|id=9282}} \| A hypothetical planet was proposed to orbit SGR 1935+2154, whose radius is smaller at {{cvt\|4.35\|km\|solar radius\|abbr=on}}.{{Cite arXiv \|eprint=2410.00635 \|class=astro-ph.HE \|first1=Yi-Xuan \|last1=Shao \|first2=Ping \|last2=Zhou \|title=GTC optical/NIR upper limits and NICER X-ray analysis of SGR J1935+2154 for the outburst in 2022 \|date=2024-10-01 \|last3=Li \|first3=Xiang-Dong \|last4=Zhang \|first4=Bin-Bin \|last5=Castro-Tirado \|first5=Alberto Javier \|last6=Wang \|first6=Pei \|last7=Li \|first7=Di \|last8=Zhang \|first8=Zeng-Hua \|last9=Zhang \|first9=Zi-Jian}}{{Cite journal \|last1=Kurban \|first1=Abdusattar \|last2=Zhou \|first2=Xia \|last3=Wang \|first3=Na \|last4=Huang \|first4=Yong-Feng \|last5=Wang \|first5=Yu-Bin \|last6=Nurmamat \|first6=Nurimangul \|date=June 2024 \|title=Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet \|journal=Astronomy & Astrophysics \|volume=686 \|pages=A87 \|doi=10.1051/0004-6361/202347828 \|arxiv=2403.13333v1 \|bibcode=2024A&A...686A..87K \|issn=0004-6361}}
Smallest stellar radius (brown dwarf) \| TVLM 513-46546b \| TVLM 513-46546 \| {{val\|0.097
0.109\|ul=solar radius}}{{Cite journal \|last1=Hallinan \|first1=G. \|last2=Antonova \|first2=A. \|last3=Doyle \|first3=J. G. \|last4=Bourke \|first4=S. \|last5=Lane \|first5=C. \|last6=Golden \|first6=A. \|date=2008-09-01 \|title=Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs \|url=https://iopscience.iop.org/article/10.1086/590360 \|journal=The Astrophysical Journal \|language=en \|volume=684 \|issue=1 \|pages=644 \|doi=10.1086/590360 \|arxiv=0805.4010 \|bibcode=2008ApJ...684..644H \|issn=0004-637X}} \| Lower than that of any brown dwarf in the NASA Exoplanet Archive.
Smallest stellar radius (main-sequence star) \| TRAPPIST-1 planets \| TRAPPIST-1 \| {{val\|0.1192\|0.0013\|ul=Solar radius}}{{Citation \|last1=Agol \|first1=Eric \|title=Refining the transit timing and photometric analysis of TRAPPIST-1: Masses, radii, densities, dynamics, and ephemerides \|date=2021-01-14 \|arxiv=2010.01074 \|last2=Dorn \|first2=Caroline \|last3=Grimm \|first3=Simon L. \|last4=Turbet \|first4=Martin \|last5=Ducrot \|first5=Elsa \|last6=Delrez \|first6=Laetitia \|last7=Gillon \|first7=Michael \|last8=Demory \|first8=Brice-Olivier \|last9=Burdanov \|first9=Artem \|journal=The Planetary Science Journal \|volume=2 \|issue=1 \|page=1 \|doi=10.3847/PSJ/abd022 \|doi-access=free \|bibcode=2021PSJ.....2....1A}} \|VB 10 (at {{Solar radius\|0.102}}){{Cite journal \|last1=Linsky \|first1=Jeffrey L. \|last2=Wood \|first2=Brian E. \|last3=Brown \|first3=Alexander \|last4=Giampapa \|first4=Mark S. \|last5=Ambruster \|first5=Carol \|date=December 1995 \|title=Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10\|journal=The Astrophysical Journal \|volume=455 \|pages=670 \|doi=10.1086/176614 \|issn=0004-637X \|bibcode=1995ApJ...455..670L \|hdl=2060/19970022983 \|hdl-access=free}} has a disproven planet candidate.
Highest stellar luminosity \| HD 220074 b \| HD 220074 \|{{val\|782.6\|20.1\|ul=Solar luminosity}} \|This is the most luminous star to host a confirmed planet that is not a potential brown dwarf. The star Mirfak, whose luminosity is {{val\|3780\|u=Solar luminosity}},{{Cite journal \|last1=McDonald \|first1=I. \|last2=Zijlstra \|first2=A. A. \|last3=Boyer \|first3=M. L. \|date=2012-11-01 \|title=Fundamental parameters and infrared excesses of Hipparcos stars \|journal=Monthly Notices of the Royal Astronomical Society \|volume=427 \|issue=1 \|pages=343–357 \|doi=10.1111/j.1365-2966.2012.21873.x \|doi-access=free \|issn=0035-8711\|arxiv=1208.2037 \|bibcode=2012MNRAS.427..343M }} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/MNRAS/427/343&HIP=15863 Alpha Persei's database entry] at VizieR. was claimed to have an orbiting planet with a minimum mass of {{Jupiter mass\|6.6 ± 0.2}}. However, the existence of the planet is doubtful. Candidate planets were reported around the cool giants V Hydrae (at {{val\|18000\|u=Solar luminosity}}),{{Cite journal \|last1=Planquart \|first1=L. \|last2=Paladini \|first2=C. \|last3=Jorissen \|first3=A. \|last4=Escorza \|first4=A. \|last5=Pantin \|first5=E. \|last6=Drevon \|first6=J. \|last7=Aringer \|first7=B. \|last8=Baron \|first8=F. \|last9=Chiavassa \|first9=A. \|last10=Cruzalèbes \|first10=P. \|last11=Danchi \|first11=W. \|last12=Beck \|first12=E. De \|last13=Groenewegen \|first13=M. a. T. \|last14=Höfner \|first14=S. \|last15=Hron \|first15=J. \|date=2024-07-01 \|title=An impressionist view of V Hydrae - When MATISSE paints asymmetric giant blobs \|journal=Astronomy & Astrophysics \|language=en \|volume=687 \|pages=A306 \|doi=10.1051/0004-6361/202348226 \|doi-access=free \|arxiv=2405.07821 \|bibcode=2024A&A...687A.306P \|issn=0004-6361}} U Equulei (at ~{{val\|6000\|u=Solar luminosity}}),{{cite journal \|arxiv=1403.7230 \|doi=10.1093/mnras/stu2383 \|title=New light on Galactic post-asymptotic giant branch stars – I. First distance catalogue \|year=2015 \|last1=Vickers \|first1=Shane B. \|last2=Frew \|first2=David J. \|last3=Parker \|first3=Quentin A. \|last4=Bojičić \|first4=Ivan S. \|journal=Monthly Notices of the Royal Astronomical Society \|volume=447\|issue=2 \|pages=1673–1691 \|doi-access=free \|bibcode=2015MNRAS.447.1673V \|s2cid=119245776 }}{{cite journal\|last=Siess\|first=Lionel\|author2=Mario Livio \|title=The accretion of brown dwarfs and planets by giant stars – II. Solar-mass stars on the red giant branch\|journal=Monthly Notices of the Royal Astronomical Society\|date=October 1999\|volume=308\|issue=4 \|pages=1133–1149 \|doi=10.1046/j.1365-8711.1999.02784.x\|doi-access=free \|arxiv = astro-ph/9905235 \|bibcode = 1999MNRAS.308.1133S \|s2cid=12893455}} R Fornacis (at {{val\|5800\|u=Solar luminosity}}), R Leonis (at {{val\|3537\|u=Solar luminosity}}), L2 Puppis (at {{val\|1490\|150\|u=Solar luminosity}}){{Cite journal \|last=Uttenthaler \|first=S. \|date=2024-12-01 \|title=The evolutionary state of the red giant star L2 Puppis \|url=https://www.aanda.org/articles/aa/full_html/2024/12/aa52173-24/aa52173-24.html \|journal=Astronomy & Astrophysics \|language=en \|volume=692 \|pages=A224 \|doi=10.1051/0004-6361/202452173 \|issn=0004-6361\|arxiv=2411.13388 }} and BD+20°2457 (at {{val\|1479\|u=Solar luminosity}}).{{Cite journal \|last1=Niedzielski \|first1=A. \|last2=Nowak \|first2=G. \|last3=Adamów \|first3=M. \|last4=Wolszczan \|first4=A. \|date=December 2009 \|title=Substellar-mass companions to the K-dwarf BD +14 4559 and the K-giants HD 240210 and BD +20 2457 \|journal=The Astrophysical Journal \|volume=707 \|issue=1 \|pages=768–777 \|doi=10.1088/0004-637X/707/1/768 \|arxiv=0906.1804 \|bibcode=2009ApJ...707..768N \|issn=0004-637X}} The host star system of the unconfirmed planet M51-ULS-1b has a luminosity of ~{{val\|261000\|u=Solar luminosity}}.{{cite arXiv \|last=Di Stefano \|first=R. \|display-authors=etal \|eprint=2009.08987 \|title=M51-ULS-1b: The First Candidate for a Planet in an External Galaxy \|class=astro-ph.HE \|date=18 September 2020 }}{{Efn\|10³⁹ erg*s⁻¹ {{=}} 10³² W {{=}} {{val\|261000\|u=Solar luminosity}}}} The stars R126, R66 and HH 1177 in the Large Magellanic Cloud have luminosities of {{val\|1400000\|u=Solar luminosity}}, {{val\|320000\|u=Solar luminosity}} and {{val\|19000\|u=Solar luminosity}} and have dust discs but no planets have been detected yet.
Lowest stellar luminosity (main-sequence star) \|TRAPPIST-1 planets \|TRAPPIST-1 \|{{Val\|0.0005495\|fmt=none\|u=Solar luminosity}} \|{{Cite journal \|last1=Agol \|first1=Eric \|last2=Dorn \|first2=Caroline \|last3=Grimm \|first3=Simon L. \|last4=Turbet \|first4=Martin \|last5=Ducrot \|first5=Elsa \|last6=Delrez \|first6=Laetitia \|last7=Gillon \|first7=Michaël \|last8=Demory \|first8=Brice-Olivier \|last9=Burdanov \|first9=Artem \|last10=Barkaoui \|first10=Khalid \|last11=Benkhaldoun \|first11=Zouhair \|last12=Bolmont \|first12=Emeline \|last13=Burgasser \|first13=Adam \|last14=Carey \|first14=Sean \|last15=de Wit \|first15=Julien \|date=2021-02-01 \|title=Refining the Transit-timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides \|journal=The Planetary Science Journal \|volume=2 \|issue=1 \|pages=1 \|doi=10.3847/PSJ/abd022 \|doi-access=free \|arxiv=2010.01074 \|bibcode=2021PSJ.....2....1A \|issn=2632-3338}}
Highest stellar rotational velocity \| Kappa Andromedae b \| Kappa Andromedae \| ~176 km/s {{citation \| last1=Royer \| first1=F. \| last2=Zorec \| first2=J. \| last3=Gómez \| first3=A. E. \| title=Rotational velocities of A-type stars. III. Velocity distributions \|journal=Astronomy and Astrophysics \| volume=463 \| issue=2 \| pages=671–682 \|date=February 2007 \| doi=10.1051/0004-6361:20065224 \| bibcode=2007A&A...463..671R \|arxiv = astro-ph/0610785 \| s2cid=18475298 }} \| The star HIP 64892 rotates slightly faster at projective velocity 178 km/s; however its orbiting companion, which weighs at {{Jupiter mass\|~29–37}} and is listed as a planet by EPE,{{cite encyclopedia \|year=2025 \|encyclopedia=Extrasolar Planets Encyclopaedia \|title=The Extrasolar Planet Encyclopaedia — HIP 64892 b. \|url=https://exoplanet.eu/catalog/hip_64892_b--6721/}} might be most likely a brown dwarf.{{Cite journal \|last1=Cheetham \|first1=A. \|last2=Bonnefoy \|first2=M. \|last3=Desidera \|first3=S. \|last4=Langlois \|first4=M. \|last5=Vigan \|first5=A. \|last6=Schmidt \|first6=T. \|last7=Olofsson \|first7=J. \|last8=Chauvin \|first8=G. \|last9=Klahr \|first9=H. \|last10=Gratton \|first10=R. \|last11=D’Orazi \|first11=V. \|last12=Henning \|first12=T. \|last13=Janson \|first13=M. \|last14=Biller \|first14=B. \|last15=Peretti \|first15=S. \|date=January 2018 \|title=Discovery of a brown dwarf companion to the star HIP 64892 \|url=https://www.aanda.org/articles/aa/abs/2018/07/aa32650-18/aa32650-18.html \|journal=Astronomy & Astrophysics \|language=en \|volume=615 \|pages=A160 \|doi=10.1051/0004-6361/201832650 \|issn=0004-6361 \|arxiv=1803.02725 \|bibcode=2018A&A...615A.160C }} The stars 51 Ophiuchi, HD 38056 and Phi Leonis rotate at {{val\|267\|5}} km/s,{{citation \| last1=Dunkin \| first1=S. K. \| last2=Barlow \| first2=M. J. \| last3=Ryan \| first3=Sean G. \| title=High-resolution spectroscopy of Vega-like stars - I. Effective temperatures, gravities and photospheric abundances \| journal=Monthly Notices of the Royal Astronomical Society \| volume=286 \| issue=3 \| pages=604–616 \| bibcode=1997MNRAS.286..604D \|date=April 1997 \| doi=10.1093/mnras/286.3.604\| doi-access=free }} ~{{val\|195}} km/s{{Cite journal \|last1=Welsh \|first1=Barry Y. \|last2=Montgomery \|first2=Sharon L. \|date=February 2018 \|title=Further detections of exocomet absorbing gas around Southern hemisphere A-type stars with known debris discs \|url=https://academic.oup.com/mnras/article/474/2/1515/4569212 \|journal=Monthly Notices of the Royal Astronomical Society \|volume=474 \|issue=2 \|pages=1515–1525 \|doi=10.1093/mnras/stx2800 \|doi-access=free \|issn=0035-8711 }} and ~{{val\|254}} km/s{{citation \| display-authors=1 \| last1=Royer \| first1=F. \| last2=Zorec \| first2=J. \| last3=Gómez \| first3=A. E. \| title=Rotational velocities of A-type stars. III. Velocity distributions \| journal=Astronomy and Astrophysics \| volume=463 \| issue=2 \| pages=671–682 \| date=February 2007 \| doi=10.1051/0004-6361:20065224 \| bibcode=2007A&A...463..671R \| arxiv=astro-ph/0610785 \| s2cid=18475298 \| postscript=.}} (respectively) and have dust discs but no planets have been detected yet.
Hottest star with a planet \| SWIFT J1756.9−2508 b \| SWIFT J1756.9−2508 \| 4,640,000 K \|{{Efn\|The cited black-body temperature {{Cite journal \|last1=Sanna \|first1=A \|last2=Pintore \|first2=F \|last3=Riggio \|first3=A \|last4=Mazzola \|first4=S M \|last5=Bozzo \|first5=E \|last6=DiSalvo \|first6=T \|last7=Ferrigno \|first7=C \|last8=Gambino \|first8=A F \|last9=Papitto \|first9=A \|last10=Iaria \|first10=R \|last11=Burderi \|first11=L \|date=2018-12-01 \|title=SWIFT J1756.9−2508: spectral and timing properties of its 2018 outburst \|url=https://academic.oup.com/mnras/article/481/2/1658/5079688 \|journal=Monthly Notices of the Royal Astronomical Society \|volume=481 \|issue=2 \|pages=1658–1666 \|doi=10.1093/mnras/sty2316 \|doi-access=free \|issn=0035-8711\|arxiv=1808.06796 }} at the poles of 0.4 keV {{=}} 400 eV corresponds to approximately 4,640,000 K (see Electronvolt#Temperature)}}
Hottest non-compact star with a planet \| NSVS 14256825 planets \| NSVS 14256825 \| 40 000 K (primary){{Cite journal \|last1=Stassun \|first1=Keivan G. \|last2=Oelkers \|first2=Ryan J. \|last3=Paegert \|first3=Martin \|last4=Torres \|first4=Guillermo \|last5=Pepper \|first5=Joshua \|last6=De Lee \|first6=Nathan \|last7=Collins \|first7=Kevin \|last8=Latham \|first8=David W. \|last9=Muirhead \|first9=Philip S. \|last10=Chittidi \|first10=Jay \|last11=Rojas-Ayala \|first11=Bárbara \|last12=Fleming \|first12=Scott W. \|last13=Rose \|first13=Mark E. \|last14=Tenenbaum \|first14=Peter \|last15=Ting \|first15=Eric B. \|date=2019-10-01 \|title=The Revised TESS Input Catalog and Candidate Target List \|journal=The Astronomical Journal \|volume=158 \|issue=4 \|pages=138 \|doi=10.3847/1538-3881/ab3467 \|doi-access=free \|arxiv=1905.10694 \|bibcode=2019AJ....158..138S \|issn=0004-6256}} \| NN Serpentis is hotter, with a temperature of 57 000 K for the primary star, but the existence of its planets is disputed.{{cite journal \|last1=Pulley \|first1=D. \|last2=Sharp \|first2=I. D. \|last3=Mallett \|first3=J. \|last4=von Harrach \|first4=S. \|date=August 2022 \|title=Eclipse timing variations in post-common envelope binaries: Are they a reliable indicator of circumbinary companions? \|journal=Monthly Notices of the Royal Astronomical Society \|volume=514 \|issue=4 \|pages=5725–5738 \|doi=10.1093/mnras/stac1676 \|doi-access=free \|arxiv=2206.06919 \|bibcode=2022MNRAS.514.5725P}} A candidate planet was found orbiting the O-type subdwarf TOI-709, whose effective temperature is higher at 50,000 K.{{Cite web \|title=TESS Project Candidates \|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=TOI \|archive-url=http://web.archive.org/web/20241227125225/https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=TOI \|archive-date=2024-12-27 \|access-date=2025-01-04 \|website=exoplanetarchive.ipac.caltech.edu \|language=en}}
Hottest main-sequence star with a planet \| b Centauri b \| b Centauri \| 18 310 ± 320 K{{cite journal \|bibcode=2021Natur.600..231J\|title=A wide-orbit giant planet in the high-mass b Centauri binary system \|last1=Janson\|first1=Markus\|last2=Gratton\|first2=Raffaele\|last3=Rodet\|first3=Laetitia\|last4=Vigan\|first4=Arthur\|last5=Bonnefoy\|first5=Mickaël\|last6=Delorme\|first6=Philippe\|last7=Mamajek\|first7=Eric E.\|last8=Reffert\|first8=Sabine\|last9=Stock\|first9=Lukas\|last10=Marleau\|first10=Gabriel-Dominique\|last11=Langlois\|first11=Maud\|last12=Chauvin\|first12=Gaël\|last13=Desidera\|first13=Silvano\|last14=Ringqvist\|first14=Simon\|last15=Mayer\|first15=Lucio\|last16=Viswanath\|first16=Gayathri\|last17=Squicciarini\|first17=Vito\|last18=Meyer\|first18=Michael R.\|last19=Samland\|first19=Matthias\|last20=Petrus\|first20=Simon\|last21=Helled\|first21=Ravit\|last22=Kenworthy\|first22=Matthew A.\|last23=Quanz\|first23=Sascha P.\|last24=Biller\|first24=Beth\|last25=Henning\|first25=Thomas\|last26=Mesa\|first26=Dino\|last27=Engler\|first27=Natalia\|last28=Carson\|first28=Joseph C.\|journal=Nature\|year=2021\|volume=600\|issue=7888\|pages=231–234\|doi=10.1038/s41586-021-04124-8\|pmid=34880428\|arxiv=2112.04833\|s2cid=245005994}} \|
Coolest star with a planet \| TRAPPIST-1 planets \| TRAPPIST-1 \| 2511 K \| Technically the primary components of Oph 162225-240515, CFBDSIR 1458+10, WISE J0336−0143 and WISE 1217+1626 are cooler, but are classified as brown dwarfs. The variable stars R Fornacis at 2100 K{{Cite book \|last=Siderud \|first=Emelie \|url=https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-423949 \|title=Dust emission modelling of AGB stars \|date=2020}} and V Camelopardalis at {{val\|2414\|86}} K were both claimed to have a planet candidate. A gas giant planet was found orbiting TVLM 513-46546,{{Cite journal \|arxiv = 2008.01595\|doi = 10.3847/1538-3881/ab9e6e\|title = An Astrometric Planetary Companion Candidate to the M9 Dwarf TVLM 513–46546\|year = 2020\|last1 = Curiel\|first1 = Salvador\|last2 = Ortiz-León\|first2 = Gisela N.\|last3 = Mioduszewski\|first3 = Amy J.\|last4 = Torres\|first4 = Rosa M.\|s2cid = 220961489\|journal = The Astronomical Journal\|volume = 160\|issue = 3\|page = 97\|bibcode = 2020AJ....160...97C \| doi-access=free }} which is an ultracool star (2242 K) located close to the brown dwarf/red dwarf mass boundary.{{Cite journal \|last1=Filippazzo \|first1=Joseph C. \|last2=Rice \|first2=Emily L. \|last3=Faherty \|first3=Jacqueline \|last4=Cruz \|first4=Kelle L. \|last5=Van Gordon \|first5=Mollie M. \|last6=Looper \|first6=Dagny L. \|date=September 2015 \|title=Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime \|arxiv=1508.01767 \|journal=The Astrophysical Journal \|volume=810 \|issue=2 \|pages=158 \|doi=10.1088/0004-637X/810/2/158 \|bibcode=2015ApJ...810..158F \|issn=1538-4357}}

class="wikitable sticky-header" style="text-align:left;"

style="background:#efefef;"| Title

! style="background:#efefef;"| Planet

! style="background:#efefef;"| Star

! style="background:#efefef;"| Data

! style="background:#efefef;"| Notes

Longest orbital period
(Longest year)

| Gliese 900 b (CW2335+0142)

| Gliese 900

| 1.27 million years{{Cite web |title=GJ 900 b - NASA Science |url=https://science.nasa.gov/exoplanet-catalog/gj-900-b/ |access-date=2024-06-20 |website=science.nasa.gov |date=31 May 2024 |language=en-US}}{{Efn|name=fn5|Assuming a circular orbit and using the Kepler's Third law}}

| COCONUTS-2b previously held this record at 1,100,000 years.{{Efn|name=fn5}}

Shortest orbital period
(Shortest year)

| GALEX 0718+3731 b

| GALEX 0718+3731

| {{nowrap|0.187 h}} (11.2 minutes)

| KOI 1843.03 has the shortest orbit around a main-sequence star (an M dwarf) at 4.25 hours.{{cite web |title=Kepler-974 |url=https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-974 |website=NASA Exoplanet Archive |publisher=Caltech |access-date=14 March 2025}}

Largest orbital separation

|Gliese 900 b (CW2335+0142)

|Gliese 900

|12 000 AU

|UCAC4 328-061594 b has an even larger orbital separation (19 000 AU), although its mass (21 M_J) is higher than the deuterium burning limit (13 M_J).

Another candidate around BD+29 5007 has an even larger orbit of about 22 100 AU. There is no consensus about its age and the resulting mass, and it could be a field brown dwarf.

The companion of ASASSN-21js has an orbit of about 13 000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass.{{Cite journal |last1=Pramono |first1=T. H. |last2=Kenworthy |first2=M. A. |last3=Boekel |first3=R. van |date=2024-08-01 |title=ASASSN-21js: A multi-year transit of a ringed disc |url=https://www.aanda.org/articles/aa/full_html/2024/08/aa50288-24/aa50288-24.html |journal=Astronomy & Astrophysics |language=en |volume=688 |pages=L11 |doi=10.1051/0004-6361/202450288 |arxiv=2408.06744 |bibcode=2024A&A...688L..11P |issn=0004-6361}}

Smallest orbital separation (smallest semi-major axis)

| GALEX 0718+3731 b

| GALEX 0718+3731

| 0.000834 AU

| TOI-6324 b has the smallest orbital separation from a main-sequence star (an M dwarf) at ~0.0043 AU.{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — TOI-6324 b. |url=https://exoplanet.eu/catalog/toi_6324_b--10860/}}

Most eccentric orbit

| HD 20782 b

| HD 20782

| 0.950

| Could alternatively be HD 28254 b with an eccentricity at {{val|0.95|0.03|0.04}}.

The possible planets HD 205577 b and SGR 1806-20 b have even higher eccentricities at {{val|0.972|0.08|0.002}} and 0.994, respectively.{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — HD 205577 b. |url=https://exoplanet.eu/catalog/hd_205577_b--7219/}}{{Citation |last1=Kurban |first1=Abdusattar |title=Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet |date=2024-03-20 |journal=Astronomy & Astrophysics |volume=686 |pages=A87 |arxiv=2403.13333 |bibcode=2024A&A...686A..87K |doi=10.1051/0004-6361/202347828 |last2=Zhou |first2=Xia |last3=Wang |first3=Na |last4=Huang |first4=Yong-Feng |last5=Wang |first5=Yu-Bin |last6=Nurmamat |first6=Nurimangul}}

The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.{{Cite encyclopedia |title=The Extrasolar Planet Encyclopaedia — VB 10 b |encyclopedia=Extrasolar Planets Encyclopaedia |url=https://exoplanet.eu/catalog/vb_10_b--550/ |access-date=2020-02-12}}

Highest orbital inclination

|HD 204313 e

|HD 204313

|{{Val|176.092|0.963|2.122|ul=deg}}

|{{Cite journal |last1=Feng |first1=Fabo |last2=Butler |first2=R. Paul |last3=Vogt |first3=Steven S. |last4=Clement | first4=Matthew S. |last5=Tinney |first5=C. G. |last6=Cui |first6=Kaiming |last7=Aizawa |first7=Masataka |last8=Jones |first8=Hugh R. A. |last9=Bailey |first9=J. |last10=Burt |first10=Jennifer |last11=Carter |first11=B. D. |last12=Crane |first12=Jeffrey D. |last13=Flammini Dotti |first13=Francesco |last14=Holden |first14=Bradford |last15=Ma |first15=Bo |date=2022-09-01 |title=3D Selection of 167 Substellar Companions to Nearby Stars |journal=The Astrophysical Journal Supplement Series |volume=262 |issue=1 |pages=21 |doi=10.3847/1538-4365/ac7e57 |doi-access=free |arxiv=2208.12720 |bibcode=2022ApJS..262...21F |issn=0067-0049}}

Lowest orbital inclination

|HD 331093 b

|HD 331093

|{{val|0.3704|p=>|u=deg}}

|{{Cite journal |last1=Dalal |first1=S. |last2=Kiefer |first2=F. |last3=Hébrard |first3=G. |last4=Sahlmann |first4=J. |last5=Sousa |first5=S. G. |last6=Forveille |first6=T. |last7=Delfosse |first7=X. |last8=Arnold |first8=L. |last9=Astudillo-Defru |first9=N. |last10=Bonfils |first10=X. |last11=Boisse |first11=I. |last12=Bouchy |first12=F. |last13=Bourrier |first13=V. |last14=Brugger |first14=B. |last15=Cortés-Zuleta |first15=P. |date=2021-07-01 |title=The SOPHIE search for northern extrasolar planets. XVII. A wealth of new objects: Six cool Jupiters, three brown dwarfs, and 16 low-mass binary stars |url=https://ui.adsabs.harvard.edu/abs/2021A&A...651A..11D |journal=Astronomy and Astrophysics |volume=651 |pages=A11 |doi=10.1051/0004-6361/202140712 |arxiv=2105.09741 |bibcode=2021A&A...651A..11D |issn=0004-6361}} HD 43197 c has the lowest orbital inclination that is not a lower limit, of {{val|11.42|5.388|3.07|u=deg}}.{{Cite web |title=Planetary Systems |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PS |access-date=2024-01-15 |website=exoplanetarchive.ipac.caltech.edu}}

Largest semi-amplitude

| WASP-18b

| WASP-18

| {{val|1814|23|24}} m/s

| {{cite journal |last1=Cortés-Zuleta |first1=Pía |last2=Rojo |first2=Patricio |display-authors=etal |date=April 2020 |title=TraMoS. V. Updated ephemeris and multi-epoch monitoring of the hot Jupiters WASP-18Ab, WASP-19b, and WASP-77Ab |journal=Astronomy & Astrophysics |volume=636 |issue= |pages=A98 |doi=10.1051/0004-6361/201936279 |arxiv=2001.11112 |bibcode=2020A&A...636A..98C |s2cid=241596186 }} The planetary-mass objects CoRoT-3b, GPX-1 b and KELT-1Ab have larger semi-amplitudes at {{val|2173|25}} m/s,{{cite web |year=2025 |website= exoplanetarchive.ipac.caltech.edu |title= CoRoT-3 Overview |url= https://exoplanetarchive.ipac.caltech.edu/overview/CoRoT-3}} {{val|2310|180}} m/s{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — GPX-1 b. |url=https://exoplanet.eu/catalog/gpx_1_b--7504/}} and {{val|4239|52}} m/s,{{Cite journal |last1=Siverd |first1=Robert J. |last2=Beatty |first2=Thomas G. |last3=Pepper |first3=Joshua |last4=Eastman |first4=Jason D. |last5=Collins |first5=Karen |last6=Bieryla |first6=Allyson |last7=Latham |first7=David W. |last8=Buchhave |first8=Lars A. |last9=Jensen |first9=Eric L. N. |last10=Crepp |first10=Justin R. |last11=Street |first11=Rachel |last12=Stassun |first12=Keivan G. |last13=Scott Gaudi |first13=B. |last14=Berlind |first14=Perry |last15=Calkins |first15=Michael L. |date=2012-12-04 |title=KELT-1b: A STRONGLY IRRADIATED, HIGHLY INFLATED, SHORT PERIOD, 27 JUPITER-MASS COMPANION TRANSITING A MID-F STAR |journal=The Astrophysical Journal |volume=761 |issue=2 |pages=123 |doi=10.1088/0004-637x/761/2/123 |issn=0004-637X|arxiv=1206.1635 }} respectively; however they are likely brown dwarfs rather than planets.{{Cite journal | title=Transiting exoplanets from the CoRoT space mission. VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert | url=https://www.aanda.org/articles/aa/full/2008/45/aa10625-08/aa10625-08.html |last1=Deleuil | first1=M. | last2=Deeg | first2=H. J. | last3=Alonso | first3=R. | last4=Bouchy | first4=F. | last5=Rouan | first5=D. | last6=Auvergne | first6=M. | last7=Baglin | first7=A. | last8=Aigrain | first8=S. | last9=Almenara | first9=J. M. | last10=Barbieri | first10=M. | last11=Barge | first11=P. | last12=Bruntt | first12=H. | last13=Bordé | first13=P. | last14=Collier Cameron | first14=A. | last15=Csizmadia | first15=S.. | last16=De La Reza | first16=R. | last17=Dvorak | first17=R. | last18=Erikson | first18=A. | last19=Fridlund | first19=M. | last20=Gandolfi | first20=D. | last21=Gillon | first21=M. | last22=Guenther | first22=E. | last23=Guillot | first23=T. | last24=Hatzes | first24=A. | last25=Hébrard | first25=G. | last26=Jorda | first26=L. | last27=Lammer | first28=A. | first29=A. | last30=Loeillet | first30=B. | last28=Léger | last29=Llebaria | first27=H. |display-authors=1 |journal=Astronomy and Astrophysics |volume=491 | issue=3 | pages=889–897 | year=2008 | arxiv=0810.0919 | bibcode=2008A&A...491..889D | doi=10.1051/0004-6361:200810625 | s2cid=8944836 }}

Smallest semi-amplitude

| Barnard's Star e

| Barnard's Star

| {{val|0.221|0.038}} m/s

Largest orbit around a single star

| COCONUTS-2b

| L 34-26

| 7506 AU

| Next largest are 2MASS J2126–8140 with 6900 AU and HD 106906 b{{cite journal |title=A Near-coplanar Stellar Flyby of the Planet Host Star HD 106906 |journal=The Astronomical Journal |first1=Robert J. |last1=De Rosa |first2=Paul |last2=Kalas |volume=157 |issue=3 |at=125 |date=February 2019 |doi=10.3847/1538-3881/ab0109 |bibcode=2019AJ....157..125D |arxiv=1902.10220|s2cid=119191779 |doi-access=free }} with ~738 AU.

UCAC4 328-061594 b has a significantly larger orbital separation (about 19,000 AU), although its mass ({{Jupiter mass|21|link=y}}){{Cite journal |last1=Rothermich |first1=Austin |last2=Faherty |first2=Jacqueline K. |last3=Bardalez-Gagliuffi |first3=Daniella |last4=Schneider |first4=Adam C. |last5=Kirkpatrick |first5=J. Davy |last6=Meisner |first6=Aaron M. |last7=Burgasser |first7=Adam J. |last8=Kuchner |first8=Marc |last9=Allers |first9=Katelyn |last10=Gagné |first10=Jonathan |last11=Caselden |first11=Dan |last12=Calamari |first12=Emily |last13=Popinchalk |first13=Mark |last14=Suárez |first14=Genaro |last15=Gerasimov |first15=Roman |date=2024-06-01 |title=89 New Ultracool Dwarf Comoving Companions Identified with the Backyard Worlds: Planet 9 Citizen Science Project |journal=The Astronomical Journal |volume=167 |issue=6 |pages=253 |arxiv=2403.04592 |bibcode=2024AJ....167..253R |doi=10.3847/1538-3881/ad324e |issn=0004-6256 |doi-access=free}} is higher than the deuterium burning limit ({{Jupiter mass|13|link=y}}).

Smallest orbit around binary star

| {{nowrap|Kepler-47b}}

| {{nowrap|Kepler-47}}

| {{val|0.2877|0.0014|0.0011|u=AU}}

|{{cite journal | journal= Science |title= Kepler-47: A Transiting Circumbinary Multi-Planet System |date= 2012|author1= Orosz, J. |author2= Welsh, W. |author3= Carter, J.|author4= Fabrycky, D. |author5= Cochran, W. | display-authors= etal | doi= 10.1126/science.1228380 | volume= 337 | issue= 6101 | pages= 1511–4 | pmid= 22933522 |bibcode= 2012Sci...337.1511O |arxiv= 1208.5489 |s2cid=44970411}}

Kepler-1521 b has a smaller orbit with semi-major axis at {{val|0.2347|0.0011|u=AU}}. The planet might be circumbinary, as the binarity of host star is suggested but not confirmed.{{Cite arXiv |last1=Kamai |first1=Ilay |last2=Perets |first2=Hagai B. |title=Too fast to be single: Tidal evolution and photometric identification of stellar and planetary companions |date=March 2025 |class=astro-ph.SR |eprint=2503.03839 }}

Smallest ratio of semi-major axis of binary star orbit to a planet orbiting one of the stars (S-type planet)

| Nu Octantis Ab

| Nu Octantis

| 2.06

| {{cite journal |author1=Ramm, D. J. |display-authors=etal |date=2016 |title=The conjectured S-type retrograde planet in ν Octantis: more evidence including four years of iodine-cell radial velocities |journal=Monthly Notices of the Royal Astronomical Society |volume=460 |issue=4 |pages=3706–3719 |arxiv=1605.06720 |bibcode=2016MNRAS.460.3706R |doi=10.1093/mnras/stw1106 |doi-access=free}}

Largest orbit around binary star

|SR 12 c

|SR 12

|≈1100 AU{{Cite journal |last1=Kuzuhara |first1=M. |last2=Tamura |first2=M. |last3=Ishii |first3=M. |last4=Kudo |first4=T. |last5=Nishiyama |first5=S. |last6=Kandori |first6=R. |date=2011-04-01 |title=The Widest-Separation Substellar Companion Candidate to a Binary T Tauri Star |url=https://iopscience.iop.org/article/10.1088/0004-6256/141/4/119 |journal=The Astronomical Journal |volume=141 |issue=4 |pages=119 |bibcode=2011AJ....141..119K |doi=10.1088/0004-6256/141/4/119 |issn=0004-6256}}

| SR 12 c has a mass of {{val|0.013|0.007|ul=Solar mass}}.

{{nowrap|DT Virginis c}}, also known as Ross 458 c, at a projected separation of ≈1200 AU, with several mass estimates below the deuterium burning limit, has a latest mass determination of {{val|27|4|ul=}} {{Jupiter mass}}.{{Cite journal |last1=Gaarn |first1=Josefine |last2=Burningham |first2=Ben |last3=Faherty |first3=Jacqueline K |last4=Visscher |first4=Channon |last5=Marley |first5=Mark S |last6=Gonzales |first6=Eileen C |last7=Calamari |first7=Emily |last8=Bardalez Gagliuffi |first8=Daniella |last9=Lupu |first9=Roxana |last10=Freedman |first10=Richard |date=2023-03-31 |title=The puzzle of the formation of T8 dwarf Ross 458c |url=https://academic.oup.com/mnras/article/521/4/5761/7078574 |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=521 |issue=4 |pages=5761–5775 |arxiv=2303.16863 |bibcode=2023MNRAS.521.5761G |doi=10.1093/mnras/stad753 |doi-access=free |issn=0035-8711}}

The binary 2MASS J0249-0557 AB has a planetary mass companion less massive than 13 M_J at a larger separation of 1950 ± 200 AU, although this companion might have formed as a brown dwarf based on the mass ratio to the primary.{{Cite journal |last1=Dupuy |first1=Trent J. |last2=Liu |first2=Michael C. |last3=Allers |first3=Katelyn N. |last4=Biller |first4=Beth A. |last5=Kratter |first5=Kaitlin M. |last6=Mann |first6=Andrew W. |last7=Shkolnik |first7=Evgenya L. |last8=Kraus |first8=Adam L. |last9=Best |first9=William M. J.|date=2018-08-01 |title=The Hawaii Infrared Parallax Program. III. 2MASS J0249-0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group |journal=The Astronomical Journal |volume=156 |issue=2 |pages=57 |arxiv=1807.05235 |bibcode=2018AJ....156...57D |doi=10.3847/1538-3881/aacbc2 |doi-access=free |issn=0004-6256}}

Largest orbit around a single star in a multiple star system

| DH Tauri b

| DH Tauri

| ≈330 AU{{Cite journal |last1=Itoh |first1=Yoichi |last2=Hayashi |first2=Masahiko |last3=Tamura |first3=Motohide |last4=Tsuji |first4=Takashi |last5=Oasa |first5=Yumiko |last6=Fukagawa |first6=Misato |last7=Hayashi |first7=Saeko S. |last8=Naoi |first8=Takahiro |last9=Ishii |first9=Miki |last10=Mayama |first10=Satoshi |last11=Morino |first11=Jun-ichi |last12=Yamashita |first12=Takuya |last13=Pyo |first13=Tae-Soo |last14=Nishikawa |first14=Takayuki |last15=Usuda |first15=Tomonori |date=2005-02-20 |title=A Young Brown Dwarf Companion to DH Tauri |url=https://iopscience.iop.org/article/10.1086/427086 |journal=The Astrophysical Journal |language=en |volume=620 |issue=2 |pages=984–993 |arxiv=astro-ph/0411177 |bibcode=2005ApJ...620..984I |doi=10.1086/427086 |issn=0004-637X}}

Largest separation between binary stars with a circumbinary planet

| SR 12 c

| SR 12

| ≈26 AU

| SR 12 c has a mass of {{val|0.013|0.007|ul=Solar mass}} at a projected separation of ≈1100 AU.
FW Tauri b orbits at a projected separation of {{val|330|30|ul=AU}} around a ≈11 AU separated binary.{{Cite journal|last1=Kraus|first1=Adam|last2=J. Ireland|first2=Michael|last3=A. Cieza|first3=Lucas|last4=Hinkley|first4=Sasha|last5=J. Dupuy|first5=Trent|last6=P. Bowler|first6=Brendan|last7=C. Liu|first7=Michael |date=2014-01-02|title=Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B|journal= The Astrophysical Journal|volume=781|issue=1|page=1311|arxiv=1311.7664|doi=10.1088/0004-637X/781/1/20|bibcode=2014ApJ...781...20K|s2cid=41086512}} It was shown to be likely a {{val|0.1

ul=Solar mass}} star surrounded by a protoplanetary disk rather than a planetary-mass companion.{{Cite journal |last1=Mora |first1=Ariel |last2=Wu |first2=Ya-Lin |last3=Bowler |first3=Brendan P. |last4=Sheehan |first4=Patrick |date=2020-01-01 |title=Measuring the Mass of the Faint Companion to FW Tau with ALMA |journal=Research Notes of the AAS |volume=4 |issue=1 |pages=9 |doi=10.3847/2515-5172/ab6852 |doi-access=free |bibcode=2020RNAAS...4....9M |issn=2515-5172}}

Largest orbit around three stars

| Gliese 900 b (CW2335+0142)

| Gliese 900

|12 000 AU

Closest orbit between stars with a planet orbiting one of the stars (S-type planet)

| {{nowrap|DMPP-3 Ab}}

| HD 42936

|1.139 AU{{cite journal |arxiv=1912.10793 |doi=10.1038/s41550-019-0972-z |title=An ablating 2.6-M_🜨 planet in an eccentric binary from the Dispersed Matter Planet Project |journal=Nature Astronomy |year=2019 |last1=Barnes |first1=John R. |last2=Haswell |first2=Carole A. |last3=Staab |first3=Daniel |last4=Anglada-Escudé |first4=Guillem |last5=Fossati |first5=Luca |last6=Doherty |first6=James P. J. |last7=Cooper |first7=Joseph |last8=Jenkins |first8=James S. |last9=Díaz |first9=Matías R. |last10=Soto |first10=Maritza G. |last11=Peña Rojas |first11=Pablo A. |volume=4 |issue=4 |pages=419–426 |s2cid=209444780}}{{Cite web |date=March 2024 |title=Multiplicity of stars with planets in the solar neighbourhood |url=https://www.aanda.org/articles/aa/pdf/forth/aa50048-24.pdf |website=aanda.org}}

| DMPP-3 Ab's semi-major axis is around 0.067 AU.

Closest orbit between stars with planets orbiting both the stars

| HD 133131 Ab, c and HD 133131 Bb

| HD 133131 A and HD 133131 B

|360 AU

|The outer planet of HD 133131 A has a semi-major axis of 4.79 AU while the only planet known of HD 133131 B has a semi-major axis of 6.40 AU.{{cite journal |bibcode=2016AJ....152..167T|doi=10.3847/0004-6256/152/6/167|arxiv=1608.06216|title=The Magellan PFS Planet Search Program: Radial Velocity and Stellar Abundance Analyses of the 360 AU, Metal-Poor Binary "Twins" HD 133131A & B|journal=The Astronomical Journal|volume=152|issue=6|pages=167|year=2016|last1=Teske|first1=Johanna K|last2=Shectman|first2=Stephen A|last3=Vogt|first3=Steve S|last4=Díaz|first4=Matías |last5=Butler |first5=R. Paul |last6=Crane |first6=Jeffrey D |last7=Thompson |first7=Ian B |last8=Arriagada |first8=Pamela |s2cid=118852162 |doi-access=free }}

Smallest semi-major axis ratio between consecutive planets

| Kepler-36b and Kepler-36c

| Kepler-36

| 1.11

| Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively; hence the planet c is 1.11 times further from star than b.

2MASS J1657-5343 b and 2MASS J1657-5343 c have semi-major axes of 165 AU and 180 AU, resulting in the planet c being ~1.09 times further from star than b.{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — 2MASS J1657-5343 b. |url=https://voparis-exoplanet-new.obspm.fr/catalog/2mass_j1657_5343_b--9993/}}{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — 2MASS J1657-5343 c. |url=https://voparis-exoplanet-new.obspm.fr/catalog/2mass_j1657_5343_c--9994/}} Despite being listed in EPE as planets, these companions are most likely brown dwarfs based on the mass.

There have been unconfirmed detections of co-orbital pairs of exoplanet, each of which has a semi-major axis ratio of almost 1.

Largest stellar radius

| HD 220074 b

| HD 220074

| {{val|59.60|5.85|6.31|ul=Solar radius}}{{Cite Gaia DR2|2014988549785194752}}

| Other stars, such as HD 18438, Mirach and Delta Virginis are larger, but their substellar companions are more massive than the deuterium burning limit at about {{Jupiter mass|13|link=y}}, and thus might be brown dwarfs rather than exoplanets.

{{Nowrap|Candidate planets were reported around the}} red giants V Camelopardalis ({{val|716|185|u=Solar radius}}),{{Cite journal |last1=van Belle |first1=G. T. |last2=Thompson |first2=R. R. |last3=Creech-Eakman |first3=M. J. |date=September 2002 |title=Angular Size Measurements Of Mira Variable Stars At 2.2 Microns. II |arxiv=astro-ph/0210167 |journal=The Astronomical Journal |volume=124 |issue=3 |pages=1706–1715 |doi=10.1086/342282|bibcode=2002AJ....124.1706V }} R Fornacis ({{Solar radius calculator|8|0.68|type=AD|unit=y}}{{Efn|1=Determined using known angular diameter and distance.
0.008 milliarcseconds * 680 pc = diameter of 5.44 au.}}),{{Cite journal |last1=Paladini |first1=C. |last2=Sacuto |first2=S. |last3=Klotz |first3=D. |last4=Ohnaka |first4=K. |last5=Wittkowski |first5=M. |last6=Nowotny |first6=W. |last7=Jorissen |first7=A. |last8=Hron |first8=J. |date=2012-08-01 |title=Detection of an asymmetry in the envelope of the carbon Mira R Fornacis using VLTI/MIDI |url=https://www.aanda.org/articles/aa/abs/2012/08/aa19831-12/aa19831-12.html |journal=Astronomy & Astrophysics |language=en |volume=544 |pages=L5 |doi=10.1051/0004-6361/201219831 |issn=0004-6361|arxiv=1207.3910 |bibcode=2012A&A...544L...5P }}{{Cite EPE|name=R For b|access-date=July 19, 2024|id=10018}} V Hydrae ({{solar radius|430}}),{{Cite journal |last1=Salas |first1=Jesus M. |last2=Naoz |first2=Smadar |last3=Morris |first3=Mark R. |last4=Stephan |first4=Alexander P. |date=2019-08-11 |title=Unseen companions of V Hya inferred from periodic ejections |arxiv=1902.08206 |journal=Monthly Notices of the Royal Astronomical Society |volume=487 |issue=3 |pages=3029–3036 |doi=10.1093/mnras/stz1515 |doi-access=free |issn=0035-8711}} R Leonis ({{Solar radius|320-350}}){{Cite journal | arxiv=0809.0359 | author=Wiesemeyer | display-authors=etal | title=Precessing planetary magnetospheres in SiO stars?. First detection of quasi-periodic polarization fluctuations in R Leonis and V Camelopardalis| journal=Astronomy and Astrophysics | volume=498 | issue=3 | pages=801–810 | date=2009 | bibcode=2009A&A...498..801W|doi = 10.1051/0004-6361/200811242 | s2cid=14531031 }}{{Cite journal |arxiv=astro-ph/0411133 |author=Fedele |display-authors=etal |title=The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI |journal=Astronomy & Astrophysics | volume=431 |issue=3 | pages=1019–1026 | date=2005 | bibcode=2005A&A...431.1019F|doi = 10.1051/0004-6361:20042013 | s2cid=15500217}} and L2 Puppis ({{val|123|14|u=Solar radius}}).

The stars R126 and R66 in the Large Magellanic Cloud have radii of {{Solar radius|78}} and {{Solar radius|131}}{{Cite journal | last1 = Kastner | first1 = J. H. | last2 = Buchanan | first2 = C. L. | last3 = Sargent | first3 = B. | last4 = Forrest | first4 = W. J. | title = SpitzerSpectroscopy of Dusty Disks around B\e] Hypergiants in the Large Magellanic Cloud | doi = 10.1086/500804 | journal = The Astrophysical Journal | volume = 638 | pages = L29–L32 | year = 2006 | issue = 1 |bibcode = 2006ApJ...638L..29K | doi-access = free }} and have dust discs but no planets have been detected yet.

Smallest stellar radius

| PSR J1211-0633 b

| PSR J1211-0633

| {{cvt|0.0000143|solar radius|km|abbr=on}}{{cite EPE|name=PSR J1211-0633 b|id=9282}}

A hypothetical planet was proposed to orbit SGR 1935+2154, whose radius is smaller at {{cvt|4.35|km|solar radius|abbr=on}}.{{Cite arXiv |eprint=2410.00635 |class=astro-ph.HE |first1=Yi-Xuan |last1=Shao |first2=Ping |last2=Zhou |title=GTC optical/NIR upper limits and NICER X-ray analysis of SGR J1935+2154 for the outburst in 2022 |date=2024-10-01 |last3=Li |first3=Xiang-Dong |last4=Zhang |first4=Bin-Bin |last5=Castro-Tirado |first5=Alberto Javier |last6=Wang |first6=Pei |last7=Li |first7=Di |last8=Zhang |first8=Zeng-Hua |last9=Zhang |first9=Zi-Jian}}{{Cite journal |last1=Kurban |first1=Abdusattar |last2=Zhou |first2=Xia |last3=Wang |first3=Na |last4=Huang |first4=Yong-Feng |last5=Wang |first5=Yu-Bin |last6=Nurmamat |first6=Nurimangul |date=June 2024 |title=Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet |journal=Astronomy & Astrophysics |volume=686 |pages=A87 |doi=10.1051/0004-6361/202347828 |arxiv=2403.13333v1 |bibcode=2024A&A...686A..87K |issn=0004-6361}}

Smallest stellar radius (brown dwarf)

| TVLM 513-46546b

| TVLM 513-46546

| {{val|0.097

0.109|ul=solar radius}}{{Cite journal |last1=Hallinan |first1=G. |last2=Antonova |first2=A. |last3=Doyle |first3=J. G. |last4=Bourke |first4=S. |last5=Lane |first5=C. |last6=Golden |first6=A. |date=2008-09-01 |title=Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs |url=https://iopscience.iop.org/article/10.1086/590360 |journal=The Astrophysical Journal |language=en |volume=684 |issue=1 |pages=644 |doi=10.1086/590360 |arxiv=0805.4010 |bibcode=2008ApJ...684..644H |issn=0004-637X}}

| Lower than that of any brown dwarf in the NASA Exoplanet Archive.

Smallest stellar radius (main-sequence star)

| TRAPPIST-1 planets

| TRAPPIST-1

| {{val|0.1192|0.0013|ul=Solar radius}}{{Citation |last1=Agol |first1=Eric |title=Refining the transit timing and photometric analysis of TRAPPIST-1: Masses, radii, densities, dynamics, and ephemerides |date=2021-01-14 |arxiv=2010.01074 |last2=Dorn |first2=Caroline |last3=Grimm |first3=Simon L. |last4=Turbet |first4=Martin |last5=Ducrot |first5=Elsa |last6=Delrez |first6=Laetitia |last7=Gillon |first7=Michael |last8=Demory |first8=Brice-Olivier |last9=Burdanov |first9=Artem |journal=The Planetary Science Journal |volume=2 |issue=1 |page=1 |doi=10.3847/PSJ/abd022 |doi-access=free |bibcode=2021PSJ.....2....1A}}

|VB 10 (at {{Solar radius|0.102}}){{Cite journal |last1=Linsky |first1=Jeffrey L. |last2=Wood |first2=Brian E. |last3=Brown |first3=Alexander |last4=Giampapa |first4=Mark S. |last5=Ambruster |first5=Carol |date=December 1995 |title=Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10|journal=The Astrophysical Journal |volume=455 |pages=670 |doi=10.1086/176614 |issn=0004-637X |bibcode=1995ApJ...455..670L |hdl=2060/19970022983 |hdl-access=free}} has a disproven planet candidate.

Highest stellar luminosity

| HD 220074 b

| HD 220074

|{{val|782.6|20.1|ul=Solar luminosity}}

|This is the most luminous star to host a confirmed planet that is not a potential brown dwarf.

The star Mirfak, whose luminosity is {{val|3780|u=Solar luminosity}},{{Cite journal |last1=McDonald |first1=I. |last2=Zijlstra |first2=A. A. |last3=Boyer |first3=M. L. |date=2012-11-01 |title=Fundamental parameters and infrared excesses of Hipparcos stars |journal=Monthly Notices of the Royal Astronomical Society |volume=427 |issue=1 |pages=343–357 |doi=10.1111/j.1365-2966.2012.21873.x |doi-access=free |issn=0035-8711|arxiv=1208.2037 |bibcode=2012MNRAS.427..343M }} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/MNRAS/427/343&HIP=15863 Alpha Persei's database entry] at VizieR. was claimed to have an orbiting planet with a minimum mass of {{Jupiter mass|6.6 ± 0.2}}. However, the existence of the planet is doubtful.

Candidate planets were reported around the cool giants V Hydrae (at {{val|18000|u=Solar luminosity}}),{{Cite journal |last1=Planquart |first1=L. |last2=Paladini |first2=C. |last3=Jorissen |first3=A. |last4=Escorza |first4=A. |last5=Pantin |first5=E. |last6=Drevon |first6=J. |last7=Aringer |first7=B. |last8=Baron |first8=F. |last9=Chiavassa |first9=A. |last10=Cruzalèbes |first10=P. |last11=Danchi |first11=W. |last12=Beck |first12=E. De |last13=Groenewegen |first13=M. a. T. |last14=Höfner |first14=S. |last15=Hron |first15=J. |date=2024-07-01 |title=An impressionist view of V Hydrae - When MATISSE paints asymmetric giant blobs |journal=Astronomy & Astrophysics |language=en |volume=687 |pages=A306 |doi=10.1051/0004-6361/202348226 |doi-access=free |arxiv=2405.07821 |bibcode=2024A&A...687A.306P |issn=0004-6361}} U Equulei (at ~{{val|6000|u=Solar luminosity}}),{{cite journal |arxiv=1403.7230 |doi=10.1093/mnras/stu2383 |title=New light on Galactic post-asymptotic giant branch stars – I. First distance catalogue |year=2015 |last1=Vickers |first1=Shane B. |last2=Frew |first2=David J. |last3=Parker |first3=Quentin A. |last4=Bojičić |first4=Ivan S. |journal=Monthly Notices of the Royal Astronomical Society |volume=447|issue=2 |pages=1673–1691 |doi-access=free |bibcode=2015MNRAS.447.1673V |s2cid=119245776 }}{{cite journal|last=Siess|first=Lionel|author2=Mario Livio |title=The accretion of brown dwarfs and planets by giant stars – II. Solar-mass stars on the red giant branch|journal=Monthly Notices of the Royal Astronomical Society|date=October 1999|volume=308|issue=4 |pages=1133–1149 |doi=10.1046/j.1365-8711.1999.02784.x|doi-access=free |arxiv = astro-ph/9905235 |bibcode = 1999MNRAS.308.1133S |s2cid=12893455}} R Fornacis (at {{val|5800|u=Solar luminosity}}), R Leonis (at {{val|3537|u=Solar luminosity}}), L2 Puppis (at {{val|1490|150|u=Solar luminosity}}){{Cite journal |last=Uttenthaler |first=S. |date=2024-12-01 |title=The evolutionary state of the red giant star L2 Puppis |url=https://www.aanda.org/articles/aa/full_html/2024/12/aa52173-24/aa52173-24.html |journal=Astronomy & Astrophysics |language=en |volume=692 |pages=A224 |doi=10.1051/0004-6361/202452173 |issn=0004-6361|arxiv=2411.13388 }} and BD+20°2457 (at {{val|1479|u=Solar luminosity}}).{{Cite journal |last1=Niedzielski |first1=A. |last2=Nowak |first2=G. |last3=Adamów |first3=M. |last4=Wolszczan |first4=A. |date=December 2009 |title=Substellar-mass companions to the K-dwarf BD +14 4559 and the K-giants HD 240210 and BD +20 2457 |journal=The Astrophysical Journal |volume=707 |issue=1 |pages=768–777 |doi=10.1088/0004-637X/707/1/768 |arxiv=0906.1804 |bibcode=2009ApJ...707..768N |issn=0004-637X}}

The host star system of the unconfirmed planet M51-ULS-1b has a luminosity of ~{{val|261000|u=Solar luminosity}}.{{cite arXiv |last=Di Stefano |first=R. |display-authors=etal |eprint=2009.08987 |title=M51-ULS-1b: The First Candidate for a Planet in an External Galaxy |class=astro-ph.HE |date=18 September 2020 }}{{Efn|10³⁹ erg*s⁻¹ {{=}} 10³² W {{=}} {{val|261000|u=Solar luminosity}}}} The stars R126, R66 and HH 1177 in the Large Magellanic Cloud have luminosities of {{val|1400000|u=Solar luminosity}}, {{val|320000|u=Solar luminosity}} and {{val|19000|u=Solar luminosity}} and have dust discs but no planets have been detected yet.

Lowest stellar luminosity (main-sequence star)

|TRAPPIST-1 planets

|TRAPPIST-1

|{{Val|0.0005495|fmt=none|u=Solar luminosity}}

|{{Cite journal |last1=Agol |first1=Eric |last2=Dorn |first2=Caroline |last3=Grimm |first3=Simon L. |last4=Turbet |first4=Martin |last5=Ducrot |first5=Elsa |last6=Delrez |first6=Laetitia |last7=Gillon |first7=Michaël |last8=Demory |first8=Brice-Olivier |last9=Burdanov |first9=Artem |last10=Barkaoui |first10=Khalid |last11=Benkhaldoun |first11=Zouhair |last12=Bolmont |first12=Emeline |last13=Burgasser |first13=Adam |last14=Carey |first14=Sean |last15=de Wit |first15=Julien |date=2021-02-01 |title=Refining the Transit-timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides |journal=The Planetary Science Journal |volume=2 |issue=1 |pages=1 |doi=10.3847/PSJ/abd022 |doi-access=free |arxiv=2010.01074 |bibcode=2021PSJ.....2....1A |issn=2632-3338}}

Highest stellar rotational velocity

| Kappa Andromedae b

| Kappa Andromedae

| ~176 km/s {{citation | last1=Royer | first1=F. | last2=Zorec | first2=J. | last3=Gómez | first3=A. E. | title=Rotational velocities of A-type stars. III. Velocity distributions |journal=Astronomy and Astrophysics | volume=463 | issue=2 | pages=671–682 |date=February 2007 | doi=10.1051/0004-6361:20065224 | bibcode=2007A&A...463..671R |arxiv = astro-ph/0610785 |

s2cid=18475298 }}

| The star HIP 64892 rotates slightly faster at projective velocity 178 km/s; however its orbiting companion, which weighs at {{Jupiter mass|~29–37}} and is listed as a planet by EPE,{{cite encyclopedia |year=2025 |encyclopedia=Extrasolar Planets Encyclopaedia |title=The Extrasolar Planet Encyclopaedia — HIP 64892 b. |url=https://exoplanet.eu/catalog/hip_64892_b--6721/}} might be most likely a brown dwarf.{{Cite journal |last1=Cheetham |first1=A. |last2=Bonnefoy |first2=M. |last3=Desidera |first3=S. |last4=Langlois |first4=M. |last5=Vigan |first5=A. |last6=Schmidt |first6=T. |last7=Olofsson |first7=J. |last8=Chauvin |first8=G. |last9=Klahr |first9=H. |last10=Gratton |first10=R. |last11=D’Orazi |first11=V. |last12=Henning |first12=T. |last13=Janson |first13=M. |last14=Biller |first14=B. |last15=Peretti |first15=S. |date=January 2018 |title=Discovery of a brown dwarf companion to the star HIP 64892 |url=https://www.aanda.org/articles/aa/abs/2018/07/aa32650-18/aa32650-18.html |journal=Astronomy & Astrophysics |language=en |volume=615 |pages=A160 |doi=10.1051/0004-6361/201832650 |issn=0004-6361 |arxiv=1803.02725 |bibcode=2018A&A...615A.160C }}

The stars 51 Ophiuchi, HD 38056 and Phi Leonis rotate at {{val|267|5}} km/s,{{citation | last1=Dunkin | first1=S. K. | last2=Barlow | first2=M. J. | last3=Ryan | first3=Sean G. | title=High-resolution spectroscopy of Vega-like stars - I. Effective temperatures, gravities and photospheric abundances | journal=Monthly Notices of the Royal Astronomical Society | volume=286 | issue=3 | pages=604–616 | bibcode=1997MNRAS.286..604D |date=April 1997 | doi=10.1093/mnras/286.3.604| doi-access=free }} ~{{val|195}} km/s{{Cite journal |last1=Welsh |first1=Barry Y. |last2=Montgomery |first2=Sharon L. |date=February 2018 |title=Further detections of exocomet absorbing gas around Southern hemisphere A-type stars with known debris discs |url=https://academic.oup.com/mnras/article/474/2/1515/4569212 |journal=Monthly Notices of the Royal Astronomical Society |volume=474 |issue=2 |pages=1515–1525 |doi=10.1093/mnras/stx2800 |doi-access=free |issn=0035-8711 }} and ~{{val|254}} km/s{{citation

| title=Rotational velocities of A-type stars. III. Velocity distributions

| journal=Astronomy and Astrophysics

| volume=463 | issue=2 | pages=671–682 | date=February 2007

| doi=10.1051/0004-6361:20065224 | bibcode=2007A&A...463..671R

| arxiv=astro-ph/0610785 | s2cid=18475298 | postscript=.}} (respectively) and have dust discs but no planets have been detected yet.

Hottest star with a planet

| SWIFT J1756.9−2508 b

| SWIFT J1756.9−2508

| 4,640,000 K

|{{Efn|The cited black-body temperature {{Cite journal |last1=Sanna |first1=A |last2=Pintore |first2=F |last3=Riggio |first3=A |last4=Mazzola |first4=S M |last5=Bozzo |first5=E |last6=DiSalvo |first6=T |last7=Ferrigno |first7=C |last8=Gambino |first8=A F |last9=Papitto |first9=A |last10=Iaria |first10=R |last11=Burderi |first11=L |date=2018-12-01 |title=SWIFT J1756.9−2508: spectral and timing properties of its 2018 outburst |url=https://academic.oup.com/mnras/article/481/2/1658/5079688 |journal=Monthly Notices of the Royal Astronomical Society |volume=481 |issue=2 |pages=1658–1666 |doi=10.1093/mnras/sty2316 |doi-access=free |issn=0035-8711|arxiv=1808.06796 }} at the poles of 0.4 keV {{=}} 400 eV corresponds to approximately 4,640,000 K (see Electronvolt#Temperature)}}

Hottest non-compact star with a planet

| NSVS 14256825 planets

| NSVS 14256825

| 40 000 K (primary){{Cite journal |last1=Stassun |first1=Keivan G. |last2=Oelkers |first2=Ryan J. |last3=Paegert |first3=Martin |last4=Torres |first4=Guillermo |last5=Pepper |first5=Joshua |last6=De Lee |first6=Nathan |last7=Collins |first7=Kevin |last8=Latham |first8=David W. |last9=Muirhead |first9=Philip S. |last10=Chittidi |first10=Jay |last11=Rojas-Ayala |first11=Bárbara |last12=Fleming |first12=Scott W. |last13=Rose |first13=Mark E. |last14=Tenenbaum |first14=Peter |last15=Ting |first15=Eric B. |date=2019-10-01 |title=The Revised TESS Input Catalog and Candidate Target List |journal=The Astronomical Journal |volume=158 |issue=4 |pages=138 |doi=10.3847/1538-3881/ab3467 |doi-access=free |arxiv=1905.10694 |bibcode=2019AJ....158..138S |issn=0004-6256}}

| NN Serpentis is hotter, with a temperature of 57 000 K for the primary star, but the existence of its planets is disputed.{{cite journal |last1=Pulley |first1=D. |last2=Sharp |first2=I. D. |last3=Mallett |first3=J. |last4=von Harrach |first4=S. |date=August 2022 |title=Eclipse timing variations in post-common envelope binaries: Are they a reliable indicator of circumbinary companions? |journal=Monthly Notices of the Royal Astronomical Society |volume=514 |issue=4 |pages=5725–5738 |doi=10.1093/mnras/stac1676 |doi-access=free |arxiv=2206.06919 |bibcode=2022MNRAS.514.5725P}}

A candidate planet was found orbiting the O-type subdwarf TOI-709, whose effective temperature is higher at 50,000 K.{{Cite web |title=TESS Project Candidates |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=TOI |archive-url=http://web.archive.org/web/20241227125225/https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=TOI |archive-date=2024-12-27 |access-date=2025-01-04 |website=exoplanetarchive.ipac.caltech.edu |language=en}}

Hottest main-sequence star with a planet

| b Centauri b

| b Centauri

| 18 310 ± 320 K{{cite journal |bibcode=2021Natur.600..231J|title=A wide-orbit giant planet in the high-mass b Centauri binary system |last1=Janson|first1=Markus|last2=Gratton|first2=Raffaele|last3=Rodet|first3=Laetitia|last4=Vigan|first4=Arthur|last5=Bonnefoy|first5=Mickaël|last6=Delorme|first6=Philippe|last7=Mamajek|first7=Eric E.|last8=Reffert|first8=Sabine|last9=Stock|first9=Lukas|last10=Marleau|first10=Gabriel-Dominique|last11=Langlois|first11=Maud|last12=Chauvin|first12=Gaël|last13=Desidera|first13=Silvano|last14=Ringqvist|first14=Simon|last15=Mayer|first15=Lucio|last16=Viswanath|first16=Gayathri|last17=Squicciarini|first17=Vito|last18=Meyer|first18=Michael R.|last19=Samland|first19=Matthias|last20=Petrus|first20=Simon|last21=Helled|first21=Ravit|last22=Kenworthy|first22=Matthew A.|last23=Quanz|first23=Sascha P.|last24=Biller|first24=Beth|last25=Henning|first25=Thomas|last26=Mesa|first26=Dino|last27=Engler|first27=Natalia|last28=Carson|first28=Joseph C.|journal=Nature|year=2021|volume=600|issue=7888|pages=231–234|doi=10.1038/s41586-021-04124-8|pmid=34880428|arxiv=2112.04833|s2cid=245005994}}

Coolest star with a planet

| TRAPPIST-1 planets

| TRAPPIST-1

| 2511 K

| Technically the primary components of Oph 162225-240515, CFBDSIR 1458+10, WISE J0336−0143 and WISE 1217+1626 are cooler, but are classified as brown dwarfs.

The variable stars R Fornacis at 2100 K{{Cite book |last=Siderud |first=Emelie |url=https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-423949 |title=Dust emission modelling of AGB stars |date=2020}} and V Camelopardalis at {{val|2414|86}} K were both claimed to have a planet candidate.

A gas giant planet was found orbiting TVLM 513-46546,{{Cite journal |arxiv = 2008.01595|doi = 10.3847/1538-3881/ab9e6e|title = An Astrometric Planetary Companion Candidate to the M9 Dwarf TVLM 513–46546|year = 2020|last1 = Curiel|first1 = Salvador|last2 = Ortiz-León|first2 = Gisela N.|last3 = Mioduszewski|first3 = Amy J.|last4 = Torres|first4 = Rosa M.|s2cid = 220961489|journal = The Astronomical Journal|volume = 160|issue = 3|page = 97|bibcode = 2020AJ....160...97C | doi-access=free }} which is an ultracool star (2242 K) located close to the brown dwarf/red dwarf mass boundary.{{Cite journal |last1=Filippazzo |first1=Joseph C. |last2=Rice |first2=Emily L. |last3=Faherty |first3=Jacqueline |last4=Cruz |first4=Kelle L. |last5=Van Gordon |first5=Mollie M. |last6=Looper |first6=Dagny L. |date=September 2015 |title=Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime |arxiv=1508.01767 |journal=The Astrophysical Journal |volume=810 |issue=2 |pages=158 |doi=10.1088/0004-637X/810/2/158 |bibcode=2015ApJ...810..158F |issn=1538-4357}}

System characteristics

class="wikitable sticky-header"
Title ! System(s) ! Planet(s) (in order from star) ! Star(s) ! Notes
System with most planets \| Kepler-90 \| 8 \| 1 \| Tau Ceti currently has no confirmed planetary companion, although it has been proposed that the number of orbiting planets may be 8, 9 or even 10.{{cite journal\|last1=Dietrich\|first1=Jeremy\|last2=Apai \|first2=Dániel \|authorlink2=Daniel Apai\|title=An Integrated Analysis with Predictions on the Architecture of the tau Ceti Planetary System, Including a Habitable Zone Planet\|journal=The Astronomical Journal\|arxiv=2010.14675 \|date=2020-10-27\|volume=161\|page=17\|doi=10.3847/1538-3881/abc560\|s2cid=225094415 \|doi-access=free }} The four planets Tau Ceti e, f, g and h are considered as strong candidates.{{Cite journal \|last1=Feng \|first1=F. \|last2=Tuomi \|first2=M. \|last3=Jones \|first3=H. R. A. \|last4=Barnes \|first4=J. \|last5=Anglada-Escudé \|first5=G. \|last6=Vogt \|first6=S. S. \|last7=Butler \|first7=R. P. \|date=2017-09-05 \|title=Color Difference Makes a Difference: Four Planet Candidates around τ Ceti \|journal=The Astronomical Journal \|volume=154 \|issue=4 \|pages=135 \|doi=10.3847/1538-3881/aa83b4 \|doi-access=free \|arxiv=1708.02051 \|bibcode=2017AJ....154..135F \|issn=0004-6256 }} HD 10180 has six confirmed planets and potentially three more planets.{{cite journal\|last=Tuomi\|first=Mikko\|title=Evidence for 9 planets in the 10180 system\|journal=Astronomy & Astrophysics\|volume=543\|pages=A52\|date=6 April 2012\|arxiv=1204.1254\|doi=10.1051/0004-6361/201118518\|bibcode = 2012A&A...543A..52T \|s2cid=15876919}} As a reference, the Solar System has eight verified major planets, alongside multiple dwarf planets (the existence of Planet Nine is yet unconfirmed{{cite news \|last=Lawler \|first=Samantha \|title=Why astronomers now doubt there is an undiscovered 9th planet in our solar system \|url=https://theconversation.com/why-astronomers-now-doubt-there-is-an-undiscovered-9th-planet-in-our-solar-system-127598 \|date=25 May 2020 \|access-date=26 May 2020 \|archive-date=29 May 2020 \|archive-url=https://web.archive.org/web/20200529051746/https://theconversation.com/why-astronomers-now-doubt-there-is-an-undiscovered-9th-planet-in-our-solar-system-127598 \|url-status=live}}).
System with most planets in habitable zone \| TRAPPIST-1 \| 7 \| 1 \|Four planets in this system (d, e, f and g) orbit within the circumstellar habitable zone.{{Cite web\|url=https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/\|title=NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star\|work=Exoplanet Exploration: Planets Beyond our Solar System\|access-date=2017-12-14 \|date=21 February 2017 \|publisher=nasa.gov}}
System with most planets in exact orbital resonance \| HD 110067 \| 6 \| 3 \|Each consecutive pair of the planets b, c, d, e, f and g is locked in the resonance of 3:2, 3:2, 3:2, 4:3 and 4:3, respectively.{{cite journal \|last1=Luque \|first1=R. \|last2=Osborn \|first2=H.P. \|display-authors=etal \|date=29 November 2023 \|title=A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067 \|journal=Nature \|volume=623 \|issue=7989 \|pages=932–937 \|doi=10.1038/s41586-023-06692-3 \|pmid=38030780 \|arxiv=2311.17775 \|bibcode=2023Natur.623..932L}}
System with most stars \| Kepler-64 \| b \| 4 \| PH1b (Kepler-64b) has a circumbinary orbit. 30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system before later studies revealing a true mass well above the red dwarf-mass limit of 80 M_Jup.{{cite journal \| title=Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets \| last1=Kiefer \| first1=F. \| last2=Hébrard \| first2=G. \| last3=Lecavelier des Etangs \| first3=A. \| last4=Martioli \| first4=E. \| last5=Dalal \| first5=S. \| last6=Vidal-Madjar \| first6=A. \| display-authors=1 \| journal=Astronomy & Astrophysics \| volume=645 \| page= \| article-number=A7 \| date=January 2021 \| arxiv=2009.14164 \| bibcode=2021A&A...645A...7K \| bibcode-access=free \| doi=10.1051/0004-6361/202039168 \| doi-access=free \| s2cid=221995447 }} The planetary mass-companion HIP 81208 Cb will be potentially located in a quadruple star system, if the star Gaia DR3 6020420074469092608 is confirmed to be gravitationally bound to the system.{{cite journal \| display-authors=1 \|last1=Viswanath \|first1=Gayathri \| last2=Janson \|first2=Markus \| last3=Gratton \| first3=Raffaele \| last4=Squicciarini \| first4=Vito \| last5=Rodet \| first5=Laetitia \| last6=Ringqvist \| first6=Simon C. \| last7=Mamajek \| first7=Eric E. \| last8=Reffert \| first8=Sabine \| last9=Chauvin \| first9=Gaël \| last10=Delorme \| first10=Philippe \| last11=Vigan \| first11=Arthur \| last12=Bonnefoy \| first12=Mickaël \| last13=Engler \| first13=Natalia \| last14=Desidera \| first14=Silvano \| last15=Henning \| first15=Thomas \| last16=Hagelberg \| first16=Janis \| last17=Langlois \| first17=Maud \| last18=Meyer \| first18=Michael \| title=BEAST detection of a brown dwarf and a low-mass stellar companion around the young bright B star HIP 81208 \| journal=Astronomy & Astrophysics \|publisher=EDP Sciences \| volume=675 \| year=2023 \| issn=0004-6361 \| doi=10.1051/0004-6361/202346154 \| doi-access=free \| page=A54\| arxiv=2305.19122 \|bibcode=2023A&A...675A..54V }}{{Creative Commons text attribution notice\|cc=by4\|from this source=yes}} The quintuple and quadruple star systems GG Tauri and HD 98800 both have several protoplanetary disks but no planets have been detected yet.{{cite web\|url=https://www.sci-news.com/astronomy/science-ezekiels-wheel-in-wheel-binary-system-gg-tauri-a-02241.html\|title=Astronomers Examine Ezekiel-like 'Wheel in a Wheel' in Binary System GG Tauri-A\|date=30 October 2014\|work=Sci-News.com\|access-date=10 February 2017}}{{Cite journal \|title= HD 98800: a most unusual debris disc \|journal=Monthly Notices of the Royal Astronomical Society \|bibcode= 2008MNRAS.390.1377V \|last1= Verrier \|first1= P. E. \|last2= Evans \|first2= N. W. \|date= 2008 \|volume= 390 \|issue= 4 \|page= 1377 \|doi= 10.1111/j.1365-2966.2008.13854.x \|doi-access= free \|arxiv= 0807.5105 }} Similarly, the star β³ Tucanae A, located in a sextuple star system, was suggested to have a debris disk with no planets having been found.{{cite journal\|bibcode= 2012ApJ...753..147D\|doi=10.1088/0004-637X/753/2/147\|title=Herschelpacs Observations and Modeling of Debris Disks in the Tucana-Horologium Association\|year=2012\|last1=Donaldson\|first1=J. K.\|last2=Roberge\|first2=A.\|last3=Chen\|first3=C. H.\|last4=Augereau\|first4=J.-C.\|last5=Dent\|first5=W. R. F.\|last6=Eiroa\|first6=C.\|last7=Krivov\|first7=A. V.\|last8=Mathews\|first8=G. S.\|last9=Meeus\|first9=G.\|last10=Ménard\|first10=F.\|last11=Riviere-Marichalar\|first11=P.\|last12=Sandell\|first12=G.\|journal=The Astrophysical Journal\|volume=753\|issue=2\|page=147\|arxiv=1206.6358 \|hdl=10486/662289\|hdl-access=free}}
System with most stellar-like objects \| Kepler-64 \| b \| 4 \| PH1b (Kepler-64b) has a circumbinary orbit. The polar circumbinary planet 2M1510 b is located in either a tertiary or a quadruple system of brown dwarfs.{{cite journal \| last1=Triaud\|first1=Amaury H. M. J.\|last2=Burgasser\|first2=Adam J. \| last3=Burdanov\|first3=Artem\|last4=Kunovac Hodžić\|first4=Vedad \| last5=Alonso\|first5=Roi\|last6=Bardalez Gagliuffi\|first6=Daniella \| last7=Delrez\|first7=Laetitia\|last8=Demory\|first8=Brice-Olivier \| last9=de Wit\|first9=Julien\|last10=Ducrot\|first10=Elsa \| last11=Hessman\|first11=Frederic V.\|date=January 2020 \| title=An Eclipsing Substellar Binary in a Young Triple System discovered by SPECULOOS \|journal=Nature Astronomy \|volume=4 \|issue=7 \|pages=650–657 \|doi=10.1038/s41550-020-1018-2 \| language=en \|arxiv=2001.07175 \|bibcode=2020NatAs...4..650T \|s2cid=210839528}} The planetary-mass object 2MASS J04414489+2301513 b is within a quadruple system with one star and two brown dwarfs.
Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star) \| Kepler-42 \| b, c, d \| 1 \| Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively. Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively.
Multiplanetary system with largest mean semi-major axis (planets are farthest from their star) \| YSES 1 \| b, c \| 1 \| YSES 1 b and c have a semi-major axis of ~162 and ~320 AU, respectively.
Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet) \| Kepler-42 \| b, c, d \| 1 \| Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is therefore 0.0094 AU. Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. The separation between closest and furthest is therefore shorter at 0.0016 AU (239,356 km).
Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet) \| AB Pictoris \| b, c \| 1 \| AB Pictoris b and c have semi-major axises of ~190 and ~4 AU,{{Cite arXiv \|last1=Lagrange \|first1=A.-M. \|last2=Kiefer \|first2=F. \|last3=Rubini \|first3=P. \|last4=Squicciarini \|first4=V. \|last5=Chomez \|first5=A. \|last6=Milli \|first6=J. \|last7=Zurlo \|first7=A. \|last8=Bouvier \|first8=J. \|last9=Delorme \|first9=P.\|title=Searching for substellar companion candidates with Gaia. III. Search for companions to members of young associations \|date=2025-01-17 \|class=astro-ph.EP \|eprint=2501.10488 }} respectively. The separation between closest and furthest is thus around 186 AU. Two planetary-mass objects with masses slightly above the deuterium limit Mu2 Scorpii b and c (the later is unconfirmed) have semi-major axises of ~19 and ~242 AU, respectively; hence the range of semi-major axis is about 223 AU.{{citation \|last1=Squicciarini \|first1=V. \|last2=Gratton \|first2=R. \|last3=Janson \|first3=M. \|last4=Mamajek \|first4=E. E. \|last5=Chauvin \|first5=G. \|last6=Delorme \|first6=P. \|last7=Langlois \|first7=M. \|last8=Vigan \|first8=A. \|last9=Ringqvist \|first9=S. C. \|last10=Meeus \|first10=G. \|last11=Reffert\|first11=S. \|last12=Kenworthy \|first12=M. \|last13=Meyer \|first13=M. R. \|last14=Bonnefoy \|first14=M. \|last15=Bonavita \|first15=M. \|last16=Mesa \|first16=D. \|last17=Samland \|first17=M. \|last18=Desidera \|first18=S. \|last19=d'Orazi \|first19=V. \|last20=Engler \|first20=N. \|last21=Alecian \|first21=E. \|last22=Miglio \|first22=A. \|last23=Henning \|first23=T. \|last24=Quanz \|first24=S. P. \|last25=Mayer \|first25=L. \|last26=Flasseur \|first26=O. \|last27=Marleau \|first27=G.-D. \|title=A scaled-up planetary system around a supernova progenitor \|journal=Astronomy & Astrophysics \|volume=664 \|pages=A9 \|date=May 2022 \|bibcode=2022A&A...664A...9S \|doi=10.1051/0004-6361/202243675 \|arxiv=2205.02279 \|s2cid=248524983}}
System with smallest total planetary mass \| Barnard's Star \| d, b, c, e \| 1 \| The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively. For comparison, Mars has a mass of 0.105 Earth masses.
System with largest total planetary mass \| HR 8799 \| e, d, c, b \| 1 \| Four planets each having masses within the range {{Jupiter mass\|5.7 – 9.1}}. Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively. They are likely brown dwarfs. HD 81817 b and c have masses of 24.1 and ≥22.6 Jupiter masses, respectively.{{cite journal \|last1=Feng \|first1=Fabo \|last2=Butler \|first2=R. Paul \|display-authors=etal \|date=August 2022 \|title=3D Selection of 167 Substellar Companions to Nearby Stars \|journal=The Astrophysical Journal Supplement Series \|volume=262 \|issue=21 \|page=21 \|doi=10.3847/1538-4365/ac7e57 \|arxiv=2208.12720 \|bibcode=2022ApJS..262...21F\|s2cid=251864022 \|doi-access=free }} These companions are also likely brown dwarfs.
Multiplanetary system with smallest mean planetary mass \| Barnard's Star \| d, b, c, e \| 1 \| The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively. For comparison, Mars has a mass of 0.105 Earth masses.
Multiplanetary system with largest mean planetary mass \| Titawin \| b, c, d \| 2 \| The three planets b, c and d have masses of {{val\|1.70\|+0.33
0.24

class="wikitable sticky-header"

Title

! System(s)

! Planet(s) (in order from star)

! Star(s)

! Notes

System with most planets

| Kepler-90

| 8

| 1

| Tau Ceti currently has no confirmed planetary companion, although it has been proposed that the number of orbiting planets may be 8, 9 or even 10.{{cite journal|last1=Dietrich|first1=Jeremy|last2=Apai |first2=Dániel |authorlink2=Daniel Apai|title=An Integrated Analysis with Predictions on the Architecture of the tau Ceti Planetary System, Including a Habitable Zone Planet|journal=The Astronomical Journal|arxiv=2010.14675 |date=2020-10-27|volume=161|page=17|doi=10.3847/1538-3881/abc560|s2cid=225094415 |doi-access=free }} The four planets Tau Ceti e, f, g and h are considered as strong candidates.{{Cite journal |last1=Feng |first1=F. |last2=Tuomi |first2=M. |last3=Jones |first3=H. R. A. |last4=Barnes |first4=J. |last5=Anglada-Escudé |first5=G. |last6=Vogt |first6=S. S. |last7=Butler |first7=R. P. |date=2017-09-05 |title=Color Difference Makes a Difference: Four Planet Candidates around τ Ceti |journal=The Astronomical Journal |volume=154 |issue=4 |pages=135 |doi=10.3847/1538-3881/aa83b4 |doi-access=free |arxiv=1708.02051 |bibcode=2017AJ....154..135F |issn=0004-6256 }}

HD 10180 has six confirmed planets and potentially three more planets.{{cite journal|last=Tuomi|first=Mikko|title=Evidence for 9 planets in the 10180 system|journal=Astronomy & Astrophysics|volume=543|pages=A52|date=6 April 2012|arxiv=1204.1254|doi=10.1051/0004-6361/201118518|bibcode = 2012A&A...543A..52T |s2cid=15876919}}

As a reference, the Solar System has eight verified major planets, alongside multiple dwarf planets (the existence of Planet Nine is yet unconfirmed{{cite news |last=Lawler |first=Samantha |title=Why astronomers now doubt there is an undiscovered 9th planet in our solar system |url=https://theconversation.com/why-astronomers-now-doubt-there-is-an-undiscovered-9th-planet-in-our-solar-system-127598 |date=25 May 2020 |access-date=26 May 2020 |archive-date=29 May 2020 |archive-url=https://web.archive.org/web/20200529051746/https://theconversation.com/why-astronomers-now-doubt-there-is-an-undiscovered-9th-planet-in-our-solar-system-127598 |url-status=live}}).

System with most planets in habitable zone

| TRAPPIST-1

| 7

| 1

|Four planets in this system (d, e, f and g) orbit within the circumstellar habitable zone.{{Cite web|url=https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/|title=NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star|work=Exoplanet Exploration: Planets Beyond our Solar System|access-date=2017-12-14 |date=21 February 2017 |publisher=nasa.gov}}

System with most planets in exact orbital resonance

| HD 110067

| 6

| 3

|Each consecutive pair of the planets b, c, d, e, f and g is locked in the resonance of 3:2, 3:2, 3:2, 4:3 and 4:3, respectively.{{cite journal |last1=Luque |first1=R. |last2=Osborn |first2=H.P. |display-authors=etal |date=29 November 2023 |title=A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067 |journal=Nature |volume=623 |issue=7989 |pages=932–937 |doi=10.1038/s41586-023-06692-3 |pmid=38030780 |arxiv=2311.17775 |bibcode=2023Natur.623..932L}}

System with most stars

| Kepler-64

| b

| 4

| PH1b (Kepler-64b) has a circumbinary orbit.

30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system before later studies revealing a true mass well above the red dwarf-mass limit of 80 M_Jup.{{cite journal | title=Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets | last1=Kiefer | first1=F. | last2=Hébrard | first2=G. | last3=Lecavelier des Etangs | first3=A. | last4=Martioli | first4=E. | last5=Dalal | first5=S. | last6=Vidal-Madjar | first6=A. | display-authors=1 | journal=Astronomy & Astrophysics | volume=645 | page= | article-number=A7 | date=January 2021 | arxiv=2009.14164 | bibcode=2021A&A...645A...7K | bibcode-access=free | doi=10.1051/0004-6361/202039168 | doi-access=free | s2cid=221995447 }}

The planetary mass-companion HIP 81208 Cb will be potentially located in a quadruple star system, if the star Gaia DR3 6020420074469092608 is confirmed to be gravitationally bound to the system.{{cite journal | display-authors=1 |last1=Viswanath |first1=Gayathri | last2=Janson |first2=Markus | last3=Gratton | first3=Raffaele | last4=Squicciarini | first4=Vito | last5=Rodet | first5=Laetitia | last6=Ringqvist | first6=Simon C. | last7=Mamajek | first7=Eric E. | last8=Reffert | first8=Sabine | last9=Chauvin | first9=Gaël | last10=Delorme | first10=Philippe | last11=Vigan | first11=Arthur | last12=Bonnefoy | first12=Mickaël | last13=Engler | first13=Natalia | last14=Desidera | first14=Silvano | last15=Henning | first15=Thomas | last16=Hagelberg | first16=Janis | last17=Langlois | first17=Maud | last18=Meyer | first18=Michael | title=BEAST detection of a brown dwarf and a low-mass stellar companion around the young bright B star HIP 81208 | journal=Astronomy & Astrophysics |publisher=EDP Sciences | volume=675 | year=2023 | issn=0004-6361 | doi=10.1051/0004-6361/202346154 | doi-access=free | page=A54| arxiv=2305.19122 |bibcode=2023A&A...675A..54V }}{{Creative Commons text attribution notice|cc=by4|from this source=yes}}

The quintuple and quadruple star systems GG Tauri and HD 98800 both have several protoplanetary disks but no planets have been detected yet.{{cite web|url=https://www.sci-news.com/astronomy/science-ezekiels-wheel-in-wheel-binary-system-gg-tauri-a-02241.html|title=Astronomers Examine Ezekiel-like 'Wheel in a Wheel' in Binary System GG Tauri-A|date=30 October 2014|work=Sci-News.com|access-date=10 February 2017}}{{Cite journal |title= HD 98800: a most unusual debris disc |journal=Monthly Notices of the Royal Astronomical Society |bibcode= 2008MNRAS.390.1377V |last1= Verrier |first1= P. E. |last2= Evans |first2= N. W. |date= 2008 |volume= 390 |issue= 4 |page= 1377 |doi= 10.1111/j.1365-2966.2008.13854.x |doi-access= free |arxiv= 0807.5105 }} Similarly, the star β³ Tucanae A, located in a sextuple star system, was suggested to have a debris disk with no planets having been found.{{cite journal|bibcode= 2012ApJ...753..147D|doi=10.1088/0004-637X/753/2/147|title=Herschelpacs Observations and Modeling of Debris Disks in the Tucana-Horologium Association|year=2012|last1=Donaldson|first1=J. K.|last2=Roberge|first2=A.|last3=Chen|first3=C. H.|last4=Augereau|first4=J.-C.|last5=Dent|first5=W. R. F.|last6=Eiroa|first6=C.|last7=Krivov|first7=A. V.|last8=Mathews|first8=G. S.|last9=Meeus|first9=G.|last10=Ménard|first10=F.|last11=Riviere-Marichalar|first11=P.|last12=Sandell|first12=G.|journal=The Astrophysical Journal|volume=753|issue=2|page=147|arxiv=1206.6358 |hdl=10486/662289|hdl-access=free}}

System with most stellar-like objects

| Kepler-64

| b

| 4

| PH1b (Kepler-64b) has a circumbinary orbit.

The polar circumbinary planet 2M1510 b is located in either a tertiary or a quadruple system of brown dwarfs.{{cite journal

| last1=Triaud|first1=Amaury H. M. J.|last2=Burgasser|first2=Adam J.

| last3=Burdanov|first3=Artem|last4=Kunovac Hodžić|first4=Vedad

| last5=Alonso|first5=Roi|last6=Bardalez Gagliuffi|first6=Daniella

| last7=Delrez|first7=Laetitia|last8=Demory|first8=Brice-Olivier

| last9=de Wit|first9=Julien|last10=Ducrot|first10=Elsa

| last11=Hessman|first11=Frederic V.|date=January 2020

| title=An Eclipsing Substellar Binary in a Young Triple System discovered by SPECULOOS

|journal=Nature Astronomy

|volume=4 |issue=7 |pages=650–657 |doi=10.1038/s41550-020-1018-2

| language=en |arxiv=2001.07175 |bibcode=2020NatAs...4..650T |s2cid=210839528}}

The planetary-mass object 2MASS J04414489+2301513 b is within a quadruple system with one star and two brown dwarfs.

Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star)

| Kepler-42

| b, c, d

| 1

| Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively.

Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively.

Multiplanetary system with largest mean semi-major axis (planets are farthest from their star)

| YSES 1

| b, c

| 1

| YSES 1 b and c have a semi-major axis of ~162 and ~320 AU, respectively.

Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet)

| Kepler-42

| b, c, d

| 1

| Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is therefore 0.0094 AU.

Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. The separation between closest and furthest is therefore shorter at 0.0016 AU (239,356 km).

Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet)

| AB Pictoris

| b, c

| 1

| AB Pictoris b and c have semi-major axises of ~190 and ~4 AU,{{Cite arXiv |last1=Lagrange |first1=A.-M. |last2=Kiefer |first2=F. |last3=Rubini |first3=P. |last4=Squicciarini |first4=V. |last5=Chomez |first5=A. |last6=Milli |first6=J. |last7=Zurlo |first7=A. |last8=Bouvier |first8=J. |last9=Delorme |first9=P.|title=Searching for substellar companion candidates with Gaia. III. Search for companions to members of young associations |date=2025-01-17 |class=astro-ph.EP |eprint=2501.10488 }} respectively. The separation between closest and furthest is thus around 186 AU.

Two planetary-mass objects with masses slightly above the deuterium limit Mu2 Scorpii b and c (the later is unconfirmed) have semi-major axises of ~19 and ~242 AU, respectively; hence the range of semi-major axis is about 223 AU.{{citation |last1=Squicciarini |first1=V. |last2=Gratton |first2=R. |last3=Janson |first3=M. |last4=Mamajek |first4=E. E. |last5=Chauvin |first5=G. |last6=Delorme |first6=P. |last7=Langlois |first7=M. |last8=Vigan |first8=A. |last9=Ringqvist |first9=S. C. |last10=Meeus |first10=G. |last11=Reffert|first11=S. |last12=Kenworthy |first12=M. |last13=Meyer |first13=M. R. |last14=Bonnefoy |first14=M. |last15=Bonavita |first15=M. |last16=Mesa |first16=D. |last17=Samland |first17=M. |last18=Desidera |first18=S. |last19=d'Orazi |first19=V. |last20=Engler |first20=N. |last21=Alecian |first21=E. |last22=Miglio |first22=A. |last23=Henning |first23=T. |last24=Quanz |first24=S. P. |last25=Mayer |first25=L. |last26=Flasseur |first26=O. |last27=Marleau |first27=G.-D. |title=A scaled-up planetary system around a supernova progenitor |journal=Astronomy & Astrophysics |volume=664 |pages=A9 |date=May 2022 |bibcode=2022A&A...664A...9S |doi=10.1051/0004-6361/202243675 |arxiv=2205.02279 |s2cid=248524983}}

System with smallest total planetary mass

| Barnard's Star

| d, b, c, e

| 1

| The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively.

For comparison, Mars has a mass of 0.105 Earth masses.

System with largest total planetary mass

| HR 8799

| e, d, c, b

| 1

| Four planets each having masses within the range {{Jupiter mass|5.7 – 9.1}}.
Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively. They are likely brown dwarfs. HD 81817 b and c have masses of 24.1 and ≥22.6 Jupiter masses, respectively.{{cite journal |last1=Feng |first1=Fabo |last2=Butler |first2=R. Paul |display-authors=etal |date=August 2022 |title=3D Selection of 167 Substellar Companions to Nearby Stars |journal=The Astrophysical Journal Supplement Series |volume=262 |issue=21 |page=21 |doi=10.3847/1538-4365/ac7e57 |arxiv=2208.12720 |bibcode=2022ApJS..262...21F|s2cid=251864022 |doi-access=free }} These companions are also likely brown dwarfs.

Multiplanetary system with smallest mean planetary mass

| Barnard's Star

| d, b, c, e

| 1

| The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively.

For comparison, Mars has a mass of 0.105 Earth masses.

Multiplanetary system with largest mean planetary mass

| Titawin

| b, c, d

| 2

| The three planets b, c and d have masses of {{val|1.70|+0.33

0.24

}, {{val|14.0|+2.3|-5.3|}} and {{val|10.2|+0.7|-3.3|}} Jupiter masses, respectively. This results in a mean planetary mass of {{Jupiter mass|5.7 – 9.7}}.{{cite journal | title=Astrometry, Radial Velocity, and Photometry: The HD 128311 System Remixed with Data from HST, HET, and APT | last1=McArthur | first1=Barbara E. | display-authors=etal | journal=The Astrophysical Journal | year=2014 | volume=795 | issue=1 | page=41 | doi=10.1088/0004-637X/795/1/41 | bibcode=2014ApJ...795...41M | s2cid=122980723 | doi-access=free }}{{cite journal |display-authors=1 | first1=D. | last1=Pizkorz | first2=B. | last2=Benneke | first3=N. R. | last3=Crockett | first4=A. C. | last4=Lockwood | first5=G. A. | last5=Blake | first6=T. S. | last6=Barman | first7=C. F. | last7=Bender |first8=J. S. |last8=Carr | first9=J. A. | last9=Johnson | title=Detection of Water Vapor in the Thermal Spectrum of the Non-transiting Hot Jupiter Upsilon Andromedae b |journal=The Astronomical Journal |volume=154 | issue=2 | pages=78 | date=August 2017 |doi=10.3847/1538-3881/aa7dd8 | bibcode=2017AJ....154...78P| arxiv=1707.01534 | s2cid=19960378 | doi-access=free }} Could alternatively be the system of HR 8799, in which four planets each have masses within the range {{Jupiter mass|5.7 – 9.1}}.

Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively. They are likely brown dwarfs. HD 81817 b and c have masses of 24.1 and ≥22.6 Jupiter masses, respectively. These companions are also likely brown dwarfs.

| Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets)

| HD 37124

| b, c, d

| 1

| HD 37124 c and d are estimated to have masses of 0.652 and 0.69 Jupiter masses, respectively (hence a ratio of about 1.058 to 1).{{cite journal |

title=The California Planet Survey. III. A Possible 2:1 Resonance in the Exoplanetary Triple System HD 37124 | last1=Wright | first1=J. T. | last2=Veras | first2=Dimitri

| last3=Ford | first3=Eric B. | last4=Johnson | first4=John Asher

| last5=Marcy | first5=G. W. | last6=Howard | first6=A. W.

| last7=Isaacson | first7=H. | last8=Fischer | first8=D. A.

| last9=Spronck | first9=J. | last10=Anderson | first10=J.

| display-authors=1 | journal=The Astrophysical Journal

| volume=730 | issue=2 | pages=61–145 | year=2011 | arxiv=1101.1097 | bibcode=2011ApJ...730...93W | doi=10.1088/0004-637X/730/2/93 | s2cid=119273897 }}

| Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets)

| Gliese 676A

| d, e, b, c

| 2

| Gliese 676A c and d have a mass ratio of about 975 to 1.{{Efn|{{math| 13.49*318/4.4 {{=}} 975}}. The true mass of planet c was measured in 2022. Assuming that the minimum mass of planet d is its true mass.}} For comparison, Mercury and Jupiter have a mass ratio of 5780 to 1.

The planet KMT-2020-BLG-0414Lc and the super-Earth KMT-2020-BLG-0414Lb have a mass ratio of about 4590 to 1,{{Efn|{{math| 27*318/1.87 {{=}} 4591.4}} }} although at {{val|27.0|4.0|3.1}} Jupiter masses KMT-2020-BLG-0414Lc might or might not be considered as a brown dwarf.{{Cite EPE|name=KMT-2020-BLG-0414L c|access-date=February 9, 2025|id=7815}}{{cite journal|last1=Schneider |first1=J. |last2=Dedieu |first2=C. |last3=Le Sidaner |first3=P. |last4=Savalle |first4=R. |last5=Zolotukhin |first5=I. |title=Defining and cataloging exoplanets: The exoplanet.eu database| date=2011| volume=532| issue=79| journal=Astronomy & Astrophysics |arxiv=1106.0586| doi=10.1051/0004-6361/201116713|pages=A79 |bibcode=2011A&A...532A..79S|s2cid=55994657 }}

Notes and references

External links

WiredScience, [https://www.wired.com/wiredscience/2009/01/top-exoplanets/ Top 5 Most Extreme Exoplanets], Clara Moskowitz, 21 January 2009

*Planetary extremes

Extrasolar planet extremes

Extremes

exoplanets

List of exoplanet extremes#Planetary characteristics

Extremes from Earth's viewpoint

Planetary characteristics

Orbital characteristics

System characteristics

See also

Notes and references

External links