List of nearest stars#Distant future and past encounters
{{Short description|Stars and brown dwarfs within 20 light years of the Solar System}}
{{Use dmy dates |date=September 2021}}
File:Nearest_stars_rotating_red-green.gif
File:Angular map of fusors around Sol within 9ly (large).png objects within 9 light years (ly), arranged clockwise in hours of right ascension, and marked by distance (▬) and position (◆). Distances are marked outward from the Sun (Sol), with concentric circles indicating the distance in one ly steps. Positions are marked inward from their distance markings, connected by lines according to their declinations (doted when positive), representing the arcs of the declinations viewed edge-on. For within 12 ly see this map.]]
This list covers all known stars, white dwarfs, brown dwarfs, and sub-brown dwarfs within {{convert|20|ly|pc|abbr=off|sigfig=3|lk=on}} of the Sun. So far, 131 such objects have been found. Only 22 are bright enough to be visible without a telescope, for which the star's visible light needs to reach or exceed the dimmest brightness visible to the naked eye from Earth, which is typically around 6.5 apparent magnitude.{{cite journal
|last=Weaver |first=Harold F.
|title=The Visibility of Stars Without Optical Aid
|journal=Publications of the Astronomical Society of the Pacific
|date=1947
|volume=59
|issue=350
|pages=232–243
|bibcode=1947PASP...59..232W
|doi=10.1086/125956|doi-access=
}}
The known 131 objects are bound in 94 stellar systems. Of those, 103 are main sequence stars: 80 red dwarfs and 23 "typical" stars having greater mass. Additionally, astronomers have found 6 white dwarfs (stars that have exhausted all fusible hydrogen), 21 brown dwarfs, as well as 1 sub-brown dwarf, WISE 0855−0714 (possibly a rogue planet). The closest system is Alpha Centauri, with Proxima Centauri as the closest star in that system, at 4.2465 light-years from Earth. The brightest, most massive and most luminous object among those 131 is Sirius A, which is also the brightest star in Earth's night sky; its white dwarf companion Sirius B is the hottest object among them. The largest object within the 20 light-years is Procyon.
The Solar System, and the other stars/dwarfs listed here, are currently moving within (or near) the Local Interstellar Cloud, roughly {{convert|30|ly|pc|1|lk=on}} across. The Local Interstellar Cloud is, in turn, contained inside the Local Bubble, a cavity in the interstellar medium about {{convert|300|ly|pc|1|lk=on}} across. It contains Ursa Major and the Hyades star cluster, among others. The Local Bubble also contains the neighboring G-Cloud, which contains the stars Alpha Centauri and Altair. In the galactic context, the Local Bubble is a small part of the Orion Arm, which contains most stars that we can see without a telescope. The Orion Arm is one of the spiral arms of our Milky Way galaxy.
Astrometrics
The easiest way to determine stellar distance to the Sun for objects at these distances is parallax, which measures how much stars appear to move against background objects over the course of Earth's orbit around the Sun. As a parsec (parallax-second) is defined by the distance of an object that would appear to move exactly one second of arc against background objects, stars less than 5 parsecs away will have measured parallaxes of over 0.2 arcseconds, or 200 milliarcseconds. Determining past and future positions relies on accurate astrometric measurements of their parallax and total proper motions (how far they move across the sky due to their actual velocity relative to the Sun), along with spectroscopically determined radial velocities (their speed directly towards or away from us, which combined with proper motion defines their true movement through the sky relative to the Sun). Both of these measurements are subject to increasing and significant errors over very long time spans, especially over the several thousand-year time spans it takes for stars to noticeably move relative to each other.{{cite journal
|title=The Close Approach of Stars in the Solar Neighborhood
|last1=Matthews |first1=R. A.
|year=1994
|journal=Quarterly Journal of the Royal Astronomical Society
|volume=35
|page=1
|bibcode=1994QJRAS..35....1M}}
Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will approach the Solar System to less than 5 parsecs in the next 15 million years. Of these, 26 have a good probability to come within {{convert|1.0|pc|ly|abbr=off|sigfig=2}} and another 7 within {{convert|0.5|pc|ly|abbr=off|sigfig=2}}.{{Cite journal|last1=Bailer-Jones|first1=C. A. L.
|last2=Rybizki|first2=J.
|last3=Andrae|first3=R.
|last4=Fouesnea|first4=M.
|title=New stellar encounters discovered in the second Gaia data release
|journal=Astronomy & Astrophysics
|volume=616
|issue=37
|pages=A37
|arxiv=1805.07581
|doi=10.1051/0004-6361/201833456
|year=2018
|bibcode=2018A&A...616A..37B
|s2cid=56269929
}} This number is likely much higher, due to the sheer number of stars needed to be surveyed; a star approaching the Solar System 10 million years ago, moving at a typical Sun-relative 20–200 kilometers per second, would be 600–6,000 light-years from the Sun at present day, with millions of stars closer to the Sun. The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun.{{cite web|title=Known Close Stellar Encounters Surge in Number
|author= Hall, Shannon
|publisher=Sky and Telescope
|date=28 May 2018
|url=http://www.skyandtelescope.com/astronomy-news/close-stellar-encounters-surge/
|access-date=2 June 2018}} It is currently predicted to pass {{val|0.1696|0.0065|u=ly}} ({{val|10635|500}} au) from the Sun in {{val|1.290|0.04}} million years from the present, close enough to significantly disturb the Solar System's Oort cloud.{{cite journal
|last1=de la Fuente Marcos |first1=Raúl
|last2=de la Fuente Marcos |first2=Carlos
|title=An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced
|journal=Research Notes of the AAS
|volume= 6
|issue= 6
|pages= 136
|year = 2022
|arxiv=
|bibcode=2022RNAAS...6..136D
|doi= 10.3847/2515-5172/ac7b95|doi-access=free }}
File:Stars-within-11-light-years2.webm
File:Game routes 100pc.png luminous stars distances map within {{cvt|100|parsec|ly}}. The number in square brackets is height above or below the galactic plane. The distance between stars is colour coded:
< 25 pc: green
< 50 pc: cyan
< 75 pc: yellow
< 100 pc: orange]]
List
{{sticky header}}
| class="wikitable sortable sticky-header-multi" style="font-size:1.00em; line-height:1.5em;"
|+Key |
| style="background-color: lightblue"| {{Hash-tag|alt=visible to naked eye}}
|Visible to the unaided eye (apparent magnitude of +6.5 or brighter) |
| style="background-color: lightgreen"| {{Dollar sign}}
|Luminous star (absolute magnitude of +8.5 or brighter) |
| style="background-color:#F5F5DC"| {{Double-dagger|alt=white dwarf}} |
| style="background-color:#D8BD98"| § |
| style="background-color:#C67B30"| {{&}} |
| style="background-color: pink"| {{Asterisk}}
|Nearest in constellation |
The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not necessarily represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible color bands (U, B or V). Absolute magnitude (with electromagnetic wave, 'light' band denoted in subscript) is a measurement at a 10-parsec distance across imaginary empty space devoid of all its sparse dust and gas. Some of the parallaxes and resultant distances are rough measurements.{{cite journal
|date=September 17, 2007
|title=The One Hundred Nearest Star Systems
|journal=Research Consortium on Nearby Stars
|url=http://www.astro.gsu.edu/RECONS/TOP100.posted.htm
|access-date=2007-11-06}}
{{clear}}
| class="wikitable sortable mw-collapsible sticky-header-multi" style="font-size: 90%; position:relative"
|+Known systems within {{convert|20|ly|pc|abbr=off|sigfig=3}} ! class="unsortable" colspan="2" |Designation ! rowspan="2" data-sort-type="number" |Distance ! rowspan="2" | ! rowspan="2" |RA/Dec ! rowspan="2" |Stellar ! rowspan="2" |Mass (M☉) ! colspan="2" |Magnitude ({{nowrap|mV or mJ}}) ! rowspan="2" |Parallax ! rowspan="2" |Notes and additional |
| class="unsortable"
!Name ! data-sort-type="number" |App. ! data-sort-type="number" |Abs. |
| Solar System
| style="background-color: lightgreen" | Sun (Sol){{Dollar sign}} | 0.0000158 | {{TableTBA|N/A}} | {{TableTBA|N/A}} | style="background: {{star-color|G}};" | G2V |1 | style="background: lightblue;" | −26.74{{Hash-tag|alt=visible to naked eye}} | 4.85 | {{TableTBA|N/A}} |eight recognized planets and more dwarf planets |
| rowspan="3" | Alpha Centauri
| Proxima Centauri (C, V645 Centauri) | 4.2465 | rowspan="3" style="background-color: pink" | Cen{{Asterisk}} | {{RA|14|29|43.0}} | style="background: {{star-color|M}};" | M5.5Ve |0.122 | 11.09 | 15.53 | 768.0665 | flare star, one confirmed planet (b, 2016, and two candidate planets, (d, 2022){{cite journal|last1=Suárez Mascareño|first1=A.|last2=Faria|first2=J. P.|last3=Figueira|first3=P.|last4=Lovis|first4=C.|last5=Damasso|first5=M.|last6=González Hernández|first6=J. I.|last7=Rebolo|first7=R.|last8=Cristiano|first8=S.|last9=Pepe|first9=F.|last10=Santos|first10=N. C.|last11=Zapatero Osorio|first11=M. R.|last12=Adibekyan|first12=V.|last13=Hojjatpanah|first13=S.|last14=Sozzetti|first14=A.|last15=Murgas|first15=F.|last16=Abreu|first16=M.|display-authors=2|title=Revisiting Proxima with ESPRESSO|journal=Astronomy & Astrophysics|year=2020|volume=639|pages=A77|issn=0004-6361|arxiv=2005.12114|doi=10.1051/0004-6361/202037745|bibcode=2020A&A...639A..77S|doi-access=free }}{{cite journal|last1=Faria|first1=J. P.|last2=Suárez Mascareño|first2=A.|last3=Figueira|first3=P.|last4=Silva|first4=A. M.|last5=Damasso|first5=M.|last6=Demangeon|first6=O.|last7=Pepe|first7=F.|last8=Santos|first8=N. C.|last9=Rebolo|first9=R.|last10=Cristiani|first10=S.|last11=Adibekyan|first11=V.|last12=Alibert|first12=Y.|last13=Allart|first13=R.|last14=Barros|first14=S. C. C.|last15=Cabral|first15=A.|last16=D’Odorico|first16=V.|last17=Di Marcantonio|first17=P.|last18=Dumusque|first18=X.|last19=Ehrenreich|first19=D.|last20=González Hernández|first20=J. I.|last21=Hara|first21=N.|last22=Lillo-Box|first22=J.|last23=Lo Curto|first23=G.|last24=Lovis|first24=C.|last25=Martins|first25=C. J. A. P.|last26=Mégevand|first26=D.|last27=Mehner|first27=A.|last28=Micela|first28=G.|last29=Molaro|first29=P.|last30=Nunes|first30=N. J.|last31=Pallé|first31=E.|last32=Poretti|first32=E.|last33=Sousa|first33=S. G.|last34=Sozzetti|first34=A.|last35=Tabernero|first35=H.|last36=Udry|first36=S.|last37=Zapatero Osorio|first37=M. R. |display-authors=3|title=A candidate short-period sub-Earth orbiting Proxima Centauri|journal=Astronomy & Astrophysics|publisher=EDP Sciences|volume=658|year=2022 |doi=10.1051/0004-6361/202142337|doi-access=free|page=A115|arxiv=2202.05188 |bibcode=2022A&A...658A.115F |url=https://www.eso.org/public/archives/releases/sciencepapers/eso2202/eso2202a.pdf}} and (c, 2019){{cite web| url=https://www.nationalgeographic.com/science/2019/04/proxima-c-new-super-earth-may-orbit-star-next-door-proxima-centauri/| archive-url=https://web.archive.org/web/20190413130915/https://www.nationalgeographic.com/science/2019/04/proxima-c-new-super-earth-may-orbit-star-next-door-proxima-centauri/| url-status=dead| archive-date=13 April 2019|title=A new super-Earth may orbit the star next door|last=Drake |first=Nadia|author-link=Nadia Drake |date=12 April 2019|website=National Geographic|access-date= 21 April 2019 }} [https://www.youtube.com/watch?v=EkqpBW4h44c Video of discovery being discussed (accidentally announced?)]{{cite journal|last1=Artigau|first1=Étienne|last2=Cadieux|first2=Charles|last3=Cook|first3=Neil J.|last4=Doyon|first4=René|last5=Vandal|first5=Thomas|last6=Donati|first6=Jean-Françcois|last7=Moutou|first7=Claire|last8=Delfosse|first8=Xavier|last9=Fouqué|first9=Pascal|last10=Martioli|first10=Eder|last11=Bouchy|first11=François|last12=Parsons|first12=Jasmine|last13=Carmona|first13=Andres|last14=Dumusque|first14=Xavier|last15=Astudillo-Defru|first15=Nicola|last16=Bonfils|first16=Xavier|last17=Mignon|first17=Lucille|display-authors=5|title=Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry|journal=The Astronomical Journal|volume=164:84|issue=3|pages=18pp|arxiv=2207.13524|bibcode=2022AJ....164...84A|doi=10.3847/1538-3881/ac7ce6|doi-access=free|date=June 23, 2022|publication-date=August 8, 2022}} |
| style="background-color: lightgreen" | Rigil Kentaurus (A){{Dollar sign}}
| rowspan="2" | 4.3441 | {{RA|14|39|36.5}} | style="background: {{star-color|G}};" | G2V |1.079 | style="background: lightblue;" | 0.01{{Hash-tag|alt=visible to naked eye}} | 4.38 | one directly imaged habitable-zone planet candidate (Candidate 1) (2021) |
| style="background-color: lightgreen" | Toliman (B){{Dollar sign}}
| {{RA|14|39|35.1}} | style="background: {{star-color|K}};" | K1V |0.909 | style="background: lightblue;" | 1.34{{Hash-tag|alt=visible to naked eye}} | 5.71 | planet b refuted in 2015 |
| colspan="2" | Barnard's Star (BD+04°3561a)
| 5.9629 | style="background-color: pink" | Oph{{Asterisk}} | {{RA|17|57|48.5}} | style="background: {{star-color|M}};" |M4.0Ve |0.144 | 9.53 | 13.22 | flare star, largest-known proper motion,{{cite journal | first=E. E. | last=Barnard | author-link=Edward Emerson Barnard | date=1916 | title=A small star with large proper motion | journal=Astronomical Journal | volume=29 | issue=695 | page=181 | bibcode = 1916AJ.....29..181B | doi = 10.1086/104156 }} four confirmed planets (d, b, c, and e){{cite journal|title=A sub-Earth-mass planet orbiting Barnard's star|first1=J. I.|last1=González Hernández|first2=A.|last2=Suárez Mascareño|first3=A. M.|last3=Silva|first4=A. K.|last4=Stefanov|first5=J. P.|last5=Faria|first6=H. M.|last6=Tabernero|first7=A.|last7=Sozzetti|first8=R.|last8=Rebolo|first9=F.|last9=Pepe|first10=N. C.|last10=Santos|first11=S.|last11=Cristiani|first12=C.|last12=Lovis|first13=X.|last13=Dumusque|first14=P.|last14=Figueira|first15=J.|last15=Lillo-Box|first16=N.|last16=Nari|first17=S.|last17=Benatti|first18=M. J.|last18=Hobson|first19=A.|last19=Castro-González|first20=R.|last20=Allart|first21=V. M.|last21=Passegger|first22=M.-R.|last22=Zapatero Osorio|first23=V.|last23=Adibekyan|first24=Y.|last24=Alibert|first25=C.|last25=Allende Prieto|first26=F.|last26=Bouchy|first27=M.|last27=Damasso|first28=V.|last28=D'Odorico|first29=P.|last29=Di Marcantonio|first30=D.|last30=Ehrenreich|first31=G.|last31=Lo Curto|first32=R.|last32=Génova Santos|first33=C. J. A. P.|last33=Martins|first34=A.|last34=Mehner|first35=G.|last35=Micela|first36=P.|last36=Molaro|first37=N.|last37=Nunes15|first38=E.|last38=Palle|first39=S. G.|last39=Sousa|first40=S.|last40=Udry|display-authors=1|journal=Astronomy & Astrophysics|volume=690|date=October 2024|pages=A79 |doi=10.1051/0004-6361/202451311|arxiv=2410.00569}}{{cite web |last1=Basant |first1=Ritvik |last2=Luque |first2=Rafael |last3=Bean |first3=Jacob |last4=Seifahrt |first4=Andreas |last5=Brady |first5=Madison |last6=Zhao |first6=Lily |last7=Brown |first7=Nina |last8=Das |first8=Tanya |last9=Stürmer |first9=Julian |last10=Kasper |first10=David |last11=Gupta |first11=Rohan |last12=Stefánsson |first12=Guđmundur |title=Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO |url=https://iopscience.iop.org/article/10.3847/2041-8213/adb8d5 |website=IOPscience |publisher=American Astronomical Society |access-date=14 March 2025}} |
| rowspan="2" | Luhman 16 (WISE 1049−5319) | style="background: #D8BD98"| A§ | rowspan="2" | 6.5029 | rowspan="2" style="background-color: pink" | Vel{{Asterisk}} | rowspan="2" | {{RA|10|49|18.9}} | style="background: {{star-color|L}};" | L8±1{{cite journal|last=Luhman|first=K. L.|year=2013|title=Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun|journal=The Astrophysical Journal Letters|volume=767|issue=1|page=L1|arxiv=1303.2401|bibcode=2013ApJ...767L...1L|doi=10.1088/2041-8205/767/1/L1|s2cid=8419422}} |0.032 | 10.7 J | 14.2 J | rowspan="2" | nearest brown dwarfs |
| style="background: #D8BD98" | B§
| style="background: {{star-color|T}};" | T1±2 |0.027 | | |
| style="background: #C67B30" colspan="2" | WISE 0855−0714{{&}}
| 7.430 | style="background-color: pink" | Hya{{Asterisk}} | {{RA|08|55|10.8}} |
| 07|14|43}}
|style="background: {{star-color|Y}};" | Y4 |0.003-0.010 | 25.0 J | 28.2 J |
| colspan="2" | Wolf 359 (CN Leonis)
| 7.8558 | style="background-color: pink" | Leo{{Asterisk}} | {{RA|10|56|29.2}} | style="background: {{star-color|M}};" | M6.0V |0.090 | 13.44 | 16.55 | flare star, has 1 candidate & 1 refuted planet{{cite arXiv|last1=Tuomi|first1=M.|last2=el|first2=al.|date=2019-06-11|title=Frequency of planets orbiting M dwarfs in the Solar neighbourhood |class=astro-ph.EP|language=en|eprint=1906.04644}}{{cite journal |bibcode=2021A&A...652A..28L |title=The CARMENES search for exoplanets around M dwarfs. Mapping stellar activity indicators across the M dwarf domain |last1=Lafarga |first1=M. |last2=Ribas |first2=I. |last3=Reiners |first3=A. |last4=Quirrenbach |first4=A. |last5=Amado |first5=P. J. |last6=Caballero |first6=J. A. |last7=Azzaro |first7=M. |last8=Béjar |first8=V. J. S. |last9=Cortés-Contreras |first9=M. |last10=Dreizler |first10=S. |last11=Hatzes |first11=A. P. |last12=Henning |first12=Th. |last13=Jeffers |first13=S. V. |last14=Kaminski |first14=A. |last15=Kürster |first15=M. |last16=Montes |first16=D. |last17=Morales |first17=J. C. |last18=Oshagh |first18=M. |last19=Rodríguez-López |first19=C. |last20=Schöfer |first20=P. |last21=Schweitzer |first21=A. |last22=Zechmeister |first22=M. |journal=Astronomy and Astrophysics |year=2021 |volume=652 |page=652 |doi=10.1051/0004-6361/202140605 |arxiv=2105.13467 |s2cid=235248016 }} |
| colspan="2" | Lalande 21185 (BD+36°2147, Gliese 411, HD 95735)
| 8.3044 | style="background-color: pink" | UMa{{Asterisk}} | {{RA|11|03|20.2}} | style="background: {{star-color|M}};" | M2.0V |0.390 | 7.47 | 10.44 |
| rowspan="2" | Sirius (Alpha Canis Majoris)
| style="background-color: lightgreen" | A{{Dollar sign}} | rowspan="2" | 8.7094 | rowspan="2" style="background-color: pink" | CMa{{Asterisk}} | rowspan="2" | {{RA|06|45|08.9}} | style="background: {{star-color|A}}" | A1V |2.063 | style="background: lightblue;" | −1.46{{Hash-tag|alt=visible to naked eye}} | 1.42 | rowspan="2" | 374.4896 | rowspan="2" | brightest star in the night sky |
| style="background: #F5F5DC" | B{{Double-dagger|alt=white dwarf}}
| style="background: #F5F5DC" | DA2 |1.018 | 8.44 | 11.34 |
| rowspan="2" | Gliese 65 (Luyten 726–8)
| A (BL Ceti) | rowspan="2" | 8.724 | rowspan="2" style="background-color: pink" | Cet{{Asterisk}} | rowspan="2" | {{RA|01|39|01.3}} | style="background: {{star-color|M}};" | M5.5Ve |0.102 | 12.54 | 15.40 | rowspan="2" | 373.8443 | rowspan="2" |flare star (Archetypal member), has 1 candidate planet{{cite journal |collaboration=GRAVITY Collaboration |last1=Abuter |first1=R. |last2=Amorim |first2=A. |last3=Benisty |first3=M. |last4=Berger |first4=J.-P. |last5=Bonnet |first5=H. |last6=Bourdarot |first6=G. |last7=Bourget |first7=P. |last8=Brandner |first8=W. |display-authors=1 |date=May 2024 |title=Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY |journal=Astronomy & Astrophysics |volume=685 |issue= |pages=L9 |doi=10.1051/0004-6361/202449547 |arxiv=2404.08746 |bibcode=2024A&A...685L...9G}} |
| B (UV Ceti)
| style="background: {{star-color|M}};" | M6.0Ve |0.100 | 12.99 | 15.85 |
| colspan="2" | Ross 154 (V1216 Sagittarii)
| 9.7063 | style="background-color: pink" | Sgr{{Asterisk}} | {{RA|18|49|49.4}} | style="background: {{star-color|M}};" | M3.5Ve |0.17 | 10.43 | 13.07 | flare star |
| colspan="2" | Ross 248 (HH Andromedae)
| 10.3057 | style="background-color: pink" | And{{Asterisk}} | {{RA|23|41|54.7}} | style="background: {{star-color|M}};" | M5.5Ve |0.136 | 12.29 | 14.79 | flare star |
| colspan="2" style="background-color: lightgreen" | Epsilon Eridani (Ran){{Dollar sign}}
| 10.4749 | style="background-color: pink" | Eri{{Asterisk}} | {{RA|03|32|55.8}} | style="background: {{star-color|K}};" | K2V |0.820 | style="background: lightblue;" | 3.73{{Hash-tag|alt=visible to naked eye}} | 6.19 | 311.37 | last1=Benedict | first1=G. Fritz | last2=McArthur | first2=Barbara E. | last3=Gatewood | first3=George | last4=Nelan | first4=Edmund | last5=Cochran | first5=William D. | last6=Hatzes | first6=Artie | last7=Endl | first7=Michael | last8=Wittenmyer | first8=Robert | last9=Baliunas | first9=Sallie L. | last10=Walker | first10=Gordon A. H. | last11=Yang | first11=Stephenson | last12=Kürster | first12=Martin | last13=Els | first13=Sebastian | last14=Paulson | first14=Diane B. |date=November 2006 | title=The extrasolar planet e Eridani b – orbit and mass | journal=The Astronomical Journal | volume=132 | issue=5 | pages=2206–2218 | bibcode=2006AJ....132.2206B | doi=10.1086/508323 | arxiv=astro-ph/0610247 | s2cid=18603036 | postscript=. }} | three circumstellar disks, |
| colspan="2" | Lacaille 9352 (Gliese 887)
| 10.7241 | style="background-color: pink" | PsA{{Asterisk}} | {{RA|23|05|52.0}} | style="background: {{star-color|M}};" | M0.5V |0.486 | 7.34 | 9.75 |flare star,{{cite journal|last=Loyd|first=R. O. Parke|last2=Shkolnik|first2=Evgenya L.|last3=France|first3=Kevin| last4=Wood|first4=Brian E.|last5=Youngblood|first5=Allison|display-authors=1|title=When “Boring” Stars Flare: The Ultraviolet Activity of GJ 887, a Bright M Star Hosting Newly Discovered Planets|journal=Research Notes of the AAS|volume=4|issue=7|date=July 2020|doi=10.3847/2515-5172/aba94a|doi-access=free|page=119}} two planets, b and c, with equivocal evidence for a third in the habitable zone (2020){{citation |arxiv=2006.16372 |title=A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887 |year=2020 |doi=10.1126/science.aaz0795 |last1=Jeffers |first1=S. V. |last2=Dreizler |first2=S. |last3=Barnes |first3=J. R. |last4=Haswell |first4=C. A. |last5=Nelson |first5=R. P. |last6=Rodríguez |first6=E. |last7=López-González |first7=M. J. |last8=Morales |first8=N. |last9=Luque |first9=R. |last10=Zechmeister |first10=M. |last11=Vogt |first11=S. S. |last12=Jenkins |first12=J. S. |last13=Pallé |first13=E. |last14=Berdi Ñas |first14=Z. M.|last15=Coleman |first15=G. A. L. |last16=Díaz |first16=M. R. |last17=Ribas |first17=I. |last18=Jones |first18=H. R. A.|last19=Butler |first19=R. P. |last20=Tinney |first20=C. G. |last21=Bailey |first21=J. |last22=Carter |first22=B. D. |last23=o'Toole |first23=S. |last24=Wittenmyer |first24=R. A. |last25=Crane |first25=J. D. |last26=Feng |first26=F. |last27=Shectman |first27=S. A. |last28=Teske |first28=J. |last29=Reiners |first29=Ansgar |last30=Amado |first30=P. J.|s2cid=220075207 |journal=Science |volume=368 |issue=6498 |pages=1477–1481 |pmid=32587019 |bibcode=2020Sci...368.1477J |display-authors=9}} |
| colspan="2" | Ross 128 (FI Virginis)
| 11.0074 | style="background-color: pink" | Vir{{Asterisk}} | {{RA|11|47|44.4}} | style="background: {{star-color|M}};" | M4.0Vn |0.168 | 11.13 | 13.51 | flare star, one planet (b) (2017){{cite web|last1= ESO|title=A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs|url=https://www.eso.org/public/archives/releases/sciencepapers/eso1736/eso1736a.pdf|access-date=15 November 2017}} |
| rowspan="3" | EZ Aquarii (Gliese 866, Luyten 789-6) | A | rowspan="3" | 11.109 | rowspan="3" style="background-color: pink" | Aqr{{Asterisk}} | rowspan="3" | {{RA|22|38|33.4}} | style="background: {{star-color|M}};" | M5.0Ve |0.11 | 13.33 | 15.64 | rowspan="3" | A & B flare stars |
| B
| style="background: {{star-color|M}};" | M? |0.11 | 13.27 | 15.58 |
| C
| style="background: {{star-color|M}};" | M? |0.10 | 14.03 | 16.34 |
| rowspan="2" | Procyon (Alpha Canis Minoris)
| style="background-color: lightgreen" | A{{Dollar sign}} | rowspan="2" | 11.402 | rowspan="2" style="background-color: pink" | CMi{{Asterisk}} | rowspan="2" | {{RA|07|39|18.1}} | style="background: {{star-color|F}}" | F5IV–V |1.499 | style="background: lightblue;" | 0.38{{Hash-tag|alt=visible to naked eye}} | 2.66 | rowspan="2" | 286.05 | rowspan="2" | |
| style="background: #F5F5DC" | B{{Double-dagger|alt=white dwarf}}
| style="background: #F5F5DC" | DQZ |0.602 | 10.70 | 12.98 |
| rowspan="2" | 61 Cygni
| style="background-color: lightgreen" | A (BD+38°4343){{Dollar sign}} | rowspan="2" | 11.4039 | rowspan="2" style="background-color: pink" | Cyg{{Asterisk}} | {{RA|21|06|53.9}} | style="background: {{star-color|K}};" | K5.0V |0.70 | style="background: lightblue;" | 5.21{{Hash-tag|alt=visible to naked eye}} | 7.49 | rowspan="2" | 286.0054 | rowspan="2" | first star (besides Sun) to have its distance measured.{{cite journal | last=Bessel | first=F. W. | title=Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel | journal=Astronomische Nachrichten | date=1839 | volume=16 | issue=5–6 | pages=65–96 | language=de | bibcode=1838AN.....16...65B | quote=(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist | doi=10.1002/asna.18390160502 | url=https://zenodo.org/record/1424605 }} A parallax of 313.6 mas yields a distance of 10.4 light years |
| style="background-color: lightgreen" | B (BD+38°4344){{Dollar sign}}
| {{RA|21|06|55.3}} | style="background: {{star-color|K}};" | K7.0V |0.63 | style="background: lightblue;" | 6.03{{Hash-tag|alt=visible to naked eye}} | 8.31 |
| rowspan="2" | Struve 2398 (Gliese 725, BD+59°1915) | A (HD 173739) | rowspan="2" | 11.4908 | rowspan="2" style="background-color: pink" | Dra{{Asterisk}} | {{RA|18|42|46.7}} | style="background: {{star-color|M}};" | M3.0V |0.334 | 8.90 | 11.16 |
| B (HD 173740)
| {{RA|18|42|46.9}} | style="background: {{star-color|M}};" | M3.5V |0.248 | 9.69 | 11.95 |
| rowspan="2" | Groombridge 34 (Gliese 15) | A (GX Andromedae) | rowspan="2" | 11.6191 | rowspan="2" | And | rowspan="2" | {{RA|00|18|22.9}} | style="background: {{star-color|M}};" | M1.5V |0.38 | 8.08 | 10.32 | rowspan="2" | 280.7068 | flare star, two known planets (Ab, 2014, and Ac, 2018){{cite journal|bibcode=2018A&A...617A.104P|title=The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction|journal=Astronomy and Astrophysics|volume=617|pages=A104|last1=Pinamonti|first1=M.|last2=Damasso|first2=M.|last3=Marzari|first3=F.|last4=Sozzetti|first4=A.|last5=Desidera|first5=S.|last6=Maldonado|first6=J.|last7=Scandariato|first7=G.|last8=Affer|first8=L.|last9=Lanza|first9=A. F.|last10=Bignamini|first10=A.|last11=Bonomo|first11=A. S.|last12=Borsa|first12=F.|last13=Claudi|first13=R.|last14=Cosentino|first14=R.|last15=Giacobbe|first15=P.|last16=González-Álvarez|first16=E.|last17=González Hernández|first17=J. I.|last18=Gratton|first18=R.|last19=Leto|first19=G.|last20=Malavolta|first20=L.|last21=Martinez Fiorenzano|first21=A.|last22=Micela|first22=G.|last23=Molinari|first23=E.|last24=Pagano|first24=I.|last25=Pedani|first25=M.|last26=Perger|first26=M.|last27=Piotto|first27=G.|last28=Rebolo|first28=R.|last29=Ribas|first29=I.|last30=Suárez Mascareño|first30=A.|display-authors=29|year=2018|arxiv=1804.03476|doi=10.1051/0004-6361/201732535|s2cid=54990041}} |
| B (GQ Andromedae)
| style="background: {{star-color|M}};" | M3.5V |0.15 | 11.06 | 13.30 | flare star |
| colspan="2" | DX Cancri (G 51-15)
| 11.6797 | style="background-color: pink" | Cnc{{Asterisk}} | {{RA|08|29|49.5}} | style="background: {{star-color|M}};" | M6.5Ve |0.09 | 14.78 | 16.98 | flare star |
| rowspan="3" | Epsilon Indi (CPD−57°10015) | style="background-color: lightgreen" | A{{Dollar sign}} | rowspan="3" | 11.8670 | rowspan="3" style="background-color: pink" | Ind{{Asterisk}} | {{RA|22|03|21.7}} | style="background: {{star-color|K}};" | K5Ve |0.754 | style="background: lightblue;" | 4.69{{Hash-tag|alt=visible to naked eye}} | 6.89 | rowspan="3" | 274.8431 | one planet (Ab) (2018){{Citation | title=Detection of the nearest Jupiter analog in radial velocity and astrometry data | first1=Fabo | last1=Feng | first2=Guillem | last2=Anglada-Escudé | first3=Mikko | last3=Tuomi | first4=Hugh R. A. | last4=Jones | first5=Julio | last5=Chanamé | first6=Paul R. | last6=Butler | first7=Markus | last7=Janson | journal=Monthly Notices of the Royal Astronomical Society | arxiv=1910.06804 | date=14 October 2019 | volume=490 | issue=4 | pages=5002–5016 | doi=10.1093/mnras/stz2912 | doi-access=free | bibcode=2019MNRAS.490.5002F | s2cid=204575783 }} |
| style="background: #D8BD98"| Ba§
| rowspan="2" | {{RA|22|04|10.5}} | style="background: {{star-color|T}};" | T1.0V |0.065 | 12.3 J{{cite web |title=DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs |publisher=caltech.edu |author=Chris Gelino, Davy Kirkpatrick, Adam Burgasser |url=http://ldwarf.ipac.caltech.edu/archive/version5/viewlist.php?table=ltdwarf&format=text |access-date=2012-06-10 |archive-date=13 November 2013 |archive-url=https://web.archive.org/web/20131113142759/http://ldwarf.ipac.caltech.edu/archive/version5/viewlist.php?table=ltdwarf&format=text |url-status=dead }} [http://spider.ipac.caltech.edu/staff/davy/ARCHIVE/index.shtml (main page)] {{Webarchive|url=https://web.archive.org/web/20190511221033/http://spider.ipac.caltech.edu/staff/davy/ARCHIVE/index.shtml |date=11 May 2019 }} | 14.5 J | |
| style="background: #D8BD98"| Bb§
| style="background: {{star-color|T}};" | T6.0V |0.050 | 15.4 J | |
| colspan="2" style="background-color: lightgreen" | Tau Ceti (BD−16°295){{Dollar sign}}
| 11.9118 | Cet | {{RA|01|44|04.1}} | style="background: {{star-color|G}};" | G8.5Vp |0.783 |style="background: lightblue;" | 3.49{{Hash-tag|alt=visible to naked eye}} | 5.68 | debris disk, |
| colspan="2" | GJ 1061 (LHS 1565)
| 11.9839 | style="background-color: pink" | Hor{{Asterisk}} | {{RA|03|35|59.7}} | style="background: {{star-color|M}};" | M5.5V |0.113 | 13.09 | 15.26 | has 3 known planets (2019){{Cite journal |journal=Monthly Notices of the Royal Astronomical Society |last1=Dreizler |first1=S. |last2=Jeffers |first2=S. V. |last3=Rodríguez |first3=E. |last4=Zechmeister |first4=M. |last5=Barnes |first5 = J.R. |last6=Haswell |first6=C.A. |last7=Coleman |first7=G. A. L. |last8=Lalitha |first8=S. |last9=Hidalgo Soto |first9=D. |last10=Strachan |first10=J.B.P. |last11=Hambsch |first11=F-J. |last12=López-González |first12=M. J. |last13=Morales |first13=N. |last14=Rodríguez López |first14=C. |last15=Berdiñas |first15=Z. M. |last16=Ribas |first16=I. |last17=Pallé |first17=E. |last18=Reiners |first18=Ansgar |last19=Anglada-Escudé |first19=G. |date=2019-08-13 |title=Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061 |doi=10.1093/mnras/staa248 |arxiv=1908.04717| s2cid=199551874 |language=en |volume=493 |issue=1 |pages=536–550|doi-access=free |bibcode=2020MNRAS.493..536D }}{{cite journal | last1 = Henry | first1 = Todd J. | last2 = Ianna | first2 = Philip A. | last3 = Kirkpatrick | first3 = J. Davy | last4 = Jahreiss | first4 = Hartmut | date = July 1997 | title = The solar neighborhood IV: discovery of the twentieth nearest star | journal = The Astronomical Journal | volume = 114 | issue = 1 | pages = 388–395 | doi = 10.1086/118482 | bibcode=1997AJ....114..388H}}{{cite journal | last1 = Henry | first1 = Todd J. | last2 = Jao | first2 = Wei-Chun | last3 = Subasavage | first3 = John P. | last4 = Beaulieu | first4 = Thomas D. | last5 = Ianna | first5 = Philip A. | last6 = Costa | first6 = Edgardo | last7 = Méndez | first7 = René A. | date = December 2006 | title = The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample | journal = The Astronomical Journal | volume = 132 | issue = 6| pages = 2360–2371 | doi = 10.1086/508233 | bibcode=2006AJ....132.2360H|arxiv = astro-ph/0608230 | s2cid = 15002841 }} |
| colspan="2" | YZ Ceti (LHS 138)
| 12.1222 | Cet | {{RA|01|12|30.6}} | style="background: {{star-color|M}};" | M4.5V |0.130 | 12.02 | 14.17 |
| colspan="2" | Luyten's Star (BD+05°1668)
| 12.3485 | CMi | {{RA|07|27|24.5}} | style="background: {{star-color|M}};" | M3.5Vn |0.26 | 9.86 | 11.97 | two planets (b, c) (2017){{cite journal | doi=10.1051/0004-6361/201630153 | last1=Astudillo-Defru | first1=Nicola | last2=Forveille | first2=Thierry | last3=Bonfils | first3=Xavier | last4=Ségransan | first4=Damien | last5=Bouchy | first5=François | last6=Delfosse | first6=Xavier | last7=Lovis | first7=Christophe | last8=Mayor | first8=Michel | last9=Murgas | first9=Felipe | last10=Pepe | first10=Francesco | last11=Santos | first11=Nuno C. | last12=Udry | first12=Stéphane | last13=Wünsche | first13=Anaël | display-authors=6 | year=2017 | title=The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293 | journal=Astronomy and Astrophysics | volume=602 | at=A88 | arxiv=1703.05386 | bibcode=2017A&A...602A..88A | s2cid=119418595 | url=https://www.aanda.org/articles/aa/full_html/2017/06/aa30153-16/aa30153-16.html }} and two suspected planets (d, e) (2019){{cite journal|last1=Pozuelos|first1=Francisco J.|last2=13 more |display-authors=1|title=GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec|journal=Astronomy & Astrophysics|volume=641|year=2020|pages=A23|doi=10.1051/0004-6361/202038047|arxiv=2006.09403|bibcode=2020A&A...641A..23P|s2cid=219721292}} |
| colspan="2" | Teegarden's Star (SO025300.5+165258)
| 12.4970 | style="background-color: pink" | Ari{{Asterisk}} | {{RA|02|53|00.9}} | style="background: {{star-color|M}};" | M6.5V |0.08 | 15.14 | 17.22 | has 3 known planets (2019, 2024){{cite journal |last1=Caballero |first1=J. A. |last2=Reiners |first2=Ansgar |last3=Ribas |first3=I. |last4=Dreizler |first4=S. |last5=Zechmeister |first5=M. |display-authors=etal |date=12 June 2019 |title=The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star |url=https://www.aanda.org/articles/aa/pdf/forth/aa35460-19.pdf |journal=Astronomy & Astrophysics |volume=627 |pages=A49 |language=en |doi=10.1051/0004-6361/201935460 |arxiv=1906.07196 |issn=0004-6361 |bibcode=2019A&A...627A..49Z |s2cid=189999121 }}{{cite journal |last1=Dreizler |first1=S. |last2=Luque |first2=R. |display-authors=etal |date=April 2024 |title=Teegarden's Star revisited: A nearby planetary system with at least three planets |journal=Astronomy & Astrophysics |volume=684 |issue= |pages=A117 |doi=10.1051/0004-6361/202348033 |arxiv=2402.00923 |bibcode=2024A&A...684A.117D}} |
| colspan="2" | Kapteyn's Star (CD−45°1841)
| 12.8308 | style="background-color: pink" | Pic{{Asterisk}} | {{RA|05|11|40.6}} | style="background: {{star-color|M}};" | M1.5VI |0.281 | 8.84 | 10.87 | two refuted planets (b and c) (2014){{cite journal|title=Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf |date=2014|arxiv=1406.0818|doi=10.1093/mnrasl/slu076 |volume=443 |journal=Monthly Notices of the Royal Astronomical Society: Letters |pages=L89–L93|bibcode = 2014MNRAS.443L..89A |hdl=2299/19219 |last1=Anglada-Escude|first1=G.|doi-access=free |s2cid=67807856|display-authors=etal}}{{cite journal|last1=Bortle|first1=Anna|last2=Fausey|first2=Hallie|last3=Ji|first3=Jinbiao|last4=Dodson-Robinson|first4=Sarah|last5=Ramirez Delgado|first5=Victor|last6=Gizis|first6=John|display-authors=1|title=A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star|journal=The Astronomical Journal|volume=161|issue=5|year=2021|pages=230|arxiv=2103.02709|doi=10.3847/1538-3881/abec89|bibcode=2021AJ....161..230B|s2cid=232110395 |doi-access=free }} |
| colspan="2" | Lacaille 8760 (AX Microscopii)
| 12.9472 | style="background-color: pink" | Mic{{Asterisk}} | {{RA|21|17|15.3}} | style="background: {{star-color|M}};" | M0.0V |0.60 | 6.67 | 8.69 | brightest M dwarf star in night sky, flare star |
| rowspan="2" | SCR 1845−6357
| A | rowspan=2 | 13.0638 | rowspan="2" style="background-color: pink" | Pav{{Asterisk}} | {{RA|18|45|05.3}} | style="background: {{star-color|M}};" | M8.5V |0.07 | 17.39 | 19.41 |
| style="background: #D8BD98"| B§
| {{RA|18|45|02.6}} | style="background: {{star-color|T}};" | T6{{Cite journal |bibcode = 2007A&A...471..655K|title = The very nearby M/T dwarf binary SCR 1845-6357|journal = Astronomy & Astrophysics|volume = 471|issue = 2|pages = 655|last1 = Kasper|first1 = M.|last2 = Biller|first2 = B. A.|last3 = Burrows|first3 = A.|last4 = Brandner|first4 = W.|last5 = Budaj|first5 = J.|last6 = Close|first6 = L. M.|year = 2007|arxiv = 0706.3824|doi = 10.1051/0004-6361:20077881|s2cid = 1860702}} | 15.3 J |
| rowspan="2" | Kruger 60 (BD+56°2783) | A | rowspan="2" | 13.0724 | rowspan="2" style="background-color: pink" | Cep{{Asterisk}} | rowspan="2" | {{RA|22|27|59.5}} | style="background: {{star-color|M}};" | M3.0V |0.271 | 9.79 | 11.76 | rowspan="2" | 249.5 | rowspan="2" | B flare star |
| B (DO Cephei)
| style="background: {{star-color|M}};" | M4.0V |0.176 | 11.41 | 13.38 |
| colspan="2" | DENIS J1048−3956
| 13.1932 | style="background-color: pink" | Ant{{Asterisk}} | {{RA|10|48|14.7}} | style="background: {{star-color|M}};" | M8.5V |0.08 | 17.39 | 19.37 | {{Cite journal |bibcode = 2005AJ....129.1954J|title = The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr−1 (MOTION Sample)|journal = The Astronomical Journal|volume = 129|issue = 4|pages = 1954|last1 = Jao|first1 = Wei-Chun|last2 = Henry|first2 = Todd J.|last3 = Subasavage|first3 = John P.|last4 = Brown|first4 = Misty A.|last5 = Ianna|first5 = Philip A.|last6 = Bartlett|first6 = Jennifer L.|author6-link=Jennifer Bartlett (astronomer)|last7 = Costa|first7 = Edgardo|last8 = Méndez|first8 = René A.|year = 2005|doi = 10.1086/428489|arxiv = astro-ph/0502167|s2cid = 16164903}}{{Cite journal |bibcode = 2005AJ....130..337C|title = The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation-First Results from the 1.5 m Telescope Program|journal = The Astronomical Journal|volume = 130|issue = 1|pages = 337|last1 = Costa|first1 = Edgardo|last2 = Méndez|first2 = René A.|last3 = Jao|first3 = W. -C.|last4 = Henry|first4 = Todd J.|last5 = Subasavage|first5 = John P.|last6 = Brown|first6 = Misty A.|last7 = Ianna|first7 = Philip A.|last8 = Bartlett|first8 = Jennifer|author8-link=Jennifer Bartlett (astronomer)|year = 2005|doi = 10.1086/430473|doi-access = free|hdl = 10533/176842|hdl-access = free}} |
| rowspan="2" | Ross 614 (V577 Monocerotis, Gliese 234) | A (LHS 1849) | rowspan="2" | 13.363 | rowspan="2" style="background-color: pink" | Mon{{Asterisk}} | rowspan="2" | {{RA|06|29|23.4}} | style="background: {{star-color|M}};" | M4.5V |0.223 | 11.15 | 13.09 | rowspan="2" | 244.07 | title=An Astrometric Study of the Low-Mass Binary Star Ross 614 | author=George Gatewood | author-link=George Gatewood | display-authors=etal | url=http://www.iop.org/EJ/article/1538-3881/125/3/1530/202454.web.pdf?request-id=b6f1cb86-b810-4d37-8eb5-4adea768585d | date=2003 | journal=The Astronomical Journal | volume=125 | issue=3 | pages=1530–1536 | doi=10.1086/346143 | bibcode=2003AJ....125.1530G | s2cid=119597659 | access-date=15 March 2022 | archive-date=19 December 2021 | archive-url=https://web.archive.org/web/20211219130826/https://www.iop.org/EJ/article/1538-3881/125/3/1530/202454.web.pdf?request-id=b6f1cb86-b810-4d37-8eb5-4adea768585d | url-status=dead }} | rowspan="2" | A flare star |
| B (LHS 1850)
| style="background: {{star-color|M}};" | M5.5V |0.111 | 14.23 | 16.17 |
| colspan="2" style="background: #D8BD98" |UGPS J0722-0540§
| 13.43 | Mon | {{RA|07|22|27.3}} | style="background: {{star-color|T}};" | T9 |0.010-0.025 | 18.45 J | 242.8 |
| colspan="2" | Wolf 1061 (Gliese 628, BD−12°4523)
| 14.0500 | Oph | {{RA|16|30|18.1}} | style="background: {{star-color|M}};" | M3.0V |0.294 | 10.07 | 11.93 | three planets (b, c, and d) (2015){{cite web | url =http://phys.org/news/2015-12-nearby-star-hosts-closest-alien.html | title =Nearby star hosts closest alien planet in the 'habitable zone' | date =December 16, 2015 | website =Phys.org | access-date =2015-12-16 | quote =The planet, more than four times the mass of the Earth, is one of three that the team detected around a red dwarf star called Wolf 1061.}} |
| colspan="2" style="background: #F5F5DC" | Van Maanen's Star (Gliese 35, LHS 7){{Double-dagger|alt=white dwarf}}
| 14.0718 | style="background-color: pink" | Psc{{Asterisk}} | {{RA|00|49|09.9}} | style="background: #F5F5DC" | DZ7 |0.67 | 12.38 | 14.21 | closest-known free-floating white dwarf, |
| colspan="2" | Gliese 1 (CD−37°15492)
| 14.1747 | style="background-color: pink" | Scl{{Asterisk}} | {{RA|00|05|24.4}} | style="background: {{star-color|M}};" | M1.5 V |0.45-0.48 | 8.55 | 10.35 | |
| colspan="2" | TZ Arietis (Gliese 83.1, L 1159–16)
| 14.5780 | Ari | {{RA|02|00|13.2}} | style="background: {{star-color|M}};" | M4.5V |0.14 | 12.27 | 14.03 |
| rowspan="2" | Wolf 424 (FL Virginis, LHS 333, Gliese 473) | A | rowspan="2" | 14.595 | rowspan="2" | Vir | rowspan="2" | {{RA|12|33|17.2}} | style="background: {{star-color|M}};" | M5.5Ve |0.143 | 13.18 | 14.97 | rowspan="2" | 223.4775 | rowspan="2" | flare stars |
| B
| style="background: {{star-color|M}};" | M7Ve |0.131 | 13.17 | 14.96 |
| colspan="2" | Gliese 687 (LHS 450, BD+68°946)
| 14.8395 | Dra | {{RA|17|36|25.9}} | style="background: {{star-color|M}};" | M3.0V |0.401 | 9.17 | 10.89 | possible flare star, two planets (b) (2014)[http://www.oklo.org/GL687.pdf The Lick–Carnegie exoplanet survey: Gliese 687 b: A Neptune-mass planet orbiting a nearby red dwarf] {{webarchive|url=https://web.archive.org/web/20140327221259/http://www.oklo.org/GL687.pdf |date=March 27, 2014 }} and (c) (2020){{citation|arxiv=2008.07998|title=Search for Nearby Earth Analogs. III. Detection of ten new planets, three planet candidates, and confirmation of three planets around eleven nearby M dwarfs|year=2020|last1=Feng|first1=Fabo|last2=Shectman|first2=Stephen A.|last3=Clement|first3=Matthew S.|last4=Vogt|first4=Steven S.|last5=Tuomi|first5=Mikko|last6=Teske|first6=Johanna K.|last7=Burt|first7=Jennifer|last8=Crane|first8=Jeffrey D.|last9=Holden|first9=Bradford|author10=Sharon Xuesong Wang|last11=Thompson|first11=Ian B.|last12=Diaz|first12=Matias R.|last13=Paul Butler|first13=R.|doi=10.3847/1538-4365/abb139|s2cid=221150644|volume=250|journal=The Astrophysical Journal Supplement Series|issue=2 |page=29 |doi-access=free |bibcode=2020ApJS..250...29F }} Accepted for publication by ApJS |
| colspan="2" | Gliese 674 (LHS 449)
| 14.8492 | style="background-color: pink" | Ara{{Asterisk}} | {{RA|17|28|39.9}} | style="background: {{star-color|M}};" | M3.0V |0.35 | 9.38 | 11.09 | one planet (b) (2007){{cite encyclopedia|url=http://exoplanet.eu/star.php?st=GJ+674|archive-url=https://web.archive.org/web/20070702185803/http://exoplanet.eu/star.php?st=GJ+674|url-status=dead|archive-date=2 July 2007|encyclopedia=Extrasolar Planets Encyclopaedia|title=The Extrasolar Planet Encyclopaedia — Catalog Listing}} |
| colspan="2" | LHS 292 (LP 731-58)
| 14.8706 | style="background-color: pink" | Sex{{Asterisk}} | {{RA|10|48|12.6}} | style="background: {{star-color|M}};" | M6.5V |0.08 | 15.60 | 17.32 | flare star |
| colspan="2" style="background: #F5F5DC" | Gliese 440 (WD 1142-645, LP 145-141){{Double-dagger|alt=white dwarf}}
| 15.1226 | style="background-color: pink" | Mus{{Asterisk}} | {{RA|11|45|42.9}} | style="background: #F5F5DC" | DQ6 |0.75 | 11.50 | 13.18 | |
| rowspan="3" | GJ 1245
| A (G 208-44 A) | rowspan="3" | 15.2001 | rowspan="3" | Cyg | {{RA|19|53|54.2}} | style="background: {{star-color|M}};" | M5.5V |0.11 | 13.46 | 15.17 | rowspan="3" | 214.5745 | rowspan="3" | flare stars |
| B (G 208-45)
| {{RA|19|53|55.2}} | style="background: {{star-color|M}};" | M6.0V |0.10 | 14.01 | 15.72 |
| C (G 208-44 B)
| {{RA|19|53|54.2}} | style="background: {{star-color|M}};" | M5.5 |0.07 | 16.75 | 18.46 |
| colspan="2" style="background: #D8BD98" | WISE 1741+2553§
| 15.22 | style="background-color: pink" | Her{{Asterisk}} | {{RA|17|41|24.2}} | style="background: {{star-color|T}};" | T9 | | 16.53 J | 18.18 J | 214.3 | doi = 10.3847/1538-4365/aaf6af | title = Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime | journal = The Astrophysical Journal Supplement | volume = 240 | issue = 19 | year = 2019 | last1 = Kirkpatrick | first1 = J. Davy | last2 = Martin | first2 = Emily C. | last3 = Smart | first3 = Richard L. | last4 = Cayago | first4 = Alfred J. | last5 = Beichman | first5 = Charles A. | last6 = Marocco | first6 = Federico | last7 = Gelino | first7 = Christopher R. | last8 = Faherty | first8 = Jacqueline K. | last9 = Cushing | first9 = Michael C. | last10 = Schneider | first10 = Adam C. | last11 = Mace | first11 = Gregory N. | last12 = Tinney | first12 = Christopher G. | last13 = Wright | first13 = Edward L. | last14 = Lowrance | first14 = Patrick J. | last15 = Ingalls | first15 = James G. | last16 = Vrba | first16 = Frederick J. | last17 = Munn | first17 = Jeffrey A. | last18 = Dahm | first18 = Scott E. | last19 = McLean | first19 = Ian S. | page = 19 |arxiv = 1812.01208 |bibcode = 2019ApJS..240...19K | s2cid = 119451195 | doi-access = free }} | |
| colspan="2" | Gliese 876 (Ross 780)
| 15.2382 | Aqr | {{RA|22|53|16.7}} | style="background: {{star-color|M}};" | M3.5V |0.37 | 10.17 | 11.81 | four planets (d (2005), c (2001), b (1998), and e (2010)){{cite journal| last1=Rivera | first1=Eugenio J.| last2=Laughlin | first2=Gregory| last3=Butler | first3=R. Paul| last4=Vogt | first4=Steven S.| last5=Haghighipour | first5=Nader| last6=Meschiari | first6=Stefano| display-authors=1| title=The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration| journal=The Astrophysical Journal| volume=719| issue=1| pages=890–899| date=July 2010 | doi=10.1088/0004-637X/719/1/890| bibcode=2010ApJ...719..890R | arxiv=1006.4244| s2cid=118707953}} |
| colspan="2" style="background: #D8BD98" | WISE 1639−6847§
| 15.336 | style="background-color: pink" | TrA{{Asterisk}} | {{RA|16|39|40.9}} |
| 68|47|46}}
| style="background: {{star-color|Y}};" | Y0.5 | | 20.57 J | 22.10 J | |
| colspan="2" | LHS 288 (Luyten 143-23)
| 15.7586 | style="background-color: pink" | Car{{Asterisk}} | {{RA|10|44|21.2}} | style="background: {{star-color|M}};" | M5.5V | 13.90 | 15.51 | |
| colspan="2" | GJ 1002
| 15.8060 | Cet | {{RA|00|06|43.8}} | style="background: {{star-color|M}};" | M5.5V |0.11 | 13.76 | 15.40 | two known planets (b & c, 2022){{cite journal |last1=Suárez Mascareño |first1=A. |last2=González-Alvarez |first2=E. |display-authors=etal |date=November 2022 |title=Two temperate Earth-mass planets orbiting the nearby star GJ 1002 |journal=Astronomy & Astrophysics |volume= 670|issue= |pages= A5|doi=10.1051/0004-6361/202244991 |arxiv=2212.07332|bibcode=2023A&A...670A...5S |s2cid=254353639 }} |
| colspan="2" style="background: #D8BD98" | DENIS 0255−4700§
| 15.877 | Eri | {{RA|02|55|03.7}} | style="background: {{star-color|L}};" | L7.5V |0.025-0.065 | 22.92 | 24.44 |
| colspan="2" style="background-color: lightgreen" | Groombridge 1618 (Gliese 380){{Dollar sign}}
| 15.8857 | UMa | {{RA|10|11|22.1}} | style="background: {{star-color|K}};" | K7.0V |0.67 | 6.59 | 8.16 | flare star, one suspected debris disk |
| rowspan="2" | Gliese 412
| A | rowspan="2" | 15.9969 | rowspan="2" | UMa | {{RA|11|05|28.6}} | style="background: {{star-color|M}};" | M1.0V |0.48 | 8.77 | 10.34 | rowspan="2" | 203.8876 | |
| B (WX Ursae Majoris)
| {{RA|11|05|30.4}} | style="background: {{star-color|M}};" | M5.5V |0.10 | 14.48 | 16.05 | flare star |
| colspan="2" | AD Leonis
| 16.1939 | Leo | {{RA|10|19|36.4}} | style="background: {{star-color|M}};" | M3.0V |0.39-0.42 | 9.32 | 10.87 | flare star, one refuted planet (b in 2020){{cite journal|last1=Carleo |first1=I.|last2=29 more |display-authors=1|year=2020|title=The GAPS Programme at TNG XXI – A GIARPS case-study of known young planetary candidates: Confirmation of HD 285507 b and refutation of AD Leo b|journal=Astronomy & Astrophysics|volume=A5|page=638|doi=10.1051/0004-6361/201937369|arxiv=2002.10562 |bibcode=2020A&A...638A...5C|s2cid=211296466}} |
| colspan="2" | Gliese 832
| 16.2005 | style="background-color: pink" | Gru{{Asterisk}} | {{RA|21|33|34.0}} | style="background: {{star-color|M}};" | M1.5 V |0.45 | 8.66 | 10.20 | possible flare star, two planets; one confirmed (b (2008)),{{cite journal | last=Bailey |first=Jeremy | display-authors=etal | title=A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832 | doi=10.1088/0004-637X/690/1/743 | bibcode=2009ApJ...690..743B | journal=The Astrophysical Journal | volume=690 | issue=1 | pages=743–747 | arxiv=0809.0172 | year=2009 |s2cid=17172233 }} and the other now refuted (c (2014)){{Cite journal|arxiv=1406.5587|title= GJ 832c: A super-earth in the habitable zone|journal= The Astrophysical Journal|volume= 791|issue= 2|pages= 114|last1= Wittenmyer|first1= R. A.|last2= Tuomi |display-authors=etal |year= 2014|doi= 10.1088/0004-637X/791/2/114|bibcode=2014ApJ...791..114W|s2cid= 12157837}}{{cite journal | last1=Gorrini | first1=P. | last2=Astudillo-Defru | first2=N. | last3=Dreizler | first3=S. | last4=Damasso | first4=M. | last5=Díaz | first5=R. F. | last6=Bonfils | first6=X. | last7=Jeffers | first7=S. V. | last8=Barnes | first8=J. R. | last9=Del Sordo | first9=F. | last10=Almenara | first10=J.-M. | last11=Artigau | first11=E. | last12=Bouchy | first12=F. | last13=Charbonneau | first13=D. | last14=Delfosse | first14=X. | last15=Doyon | first15=R. | last16=Figueira | first16=P. | last17=Forveille | first17=T. | last18=Haswell | first18=C. A. | last19=López-González | first19=M. J. | last20=Melo | first20=C. | last21=Mennickent | first21=R. E. | last22=Gaisné | first22=G. | last23=Morales | first23=N. Morales | last24=Murgas | first24=F. | last25=Pepe | first25=F. | last26=Rodríguez | first26=E. | last27=Santos | first27=N. C. | last28=Tal-Or | first28=L. | last29=Tsapras | first29=Y. | last30=Udry | first30=S.|display-authors=3 | title=Detailed stellar activity analysis and modelling of GJ 832 | journal=Astronomy & Astrophysics | publisher=EDP Sciences | volume=664 | year=2022 | issn=0004-6361 | doi=10.1051/0004-6361/202243063 |doi-access=free | page=A64| arxiv=2206.07552 | bibcode=2022A&A...664A..64G }} |
| colspan = '2' | Gliese 682 (CD-44 11909)
| 16.3328 | style="background-color: pink" | Sco{{Asterisk}} | {{RA|17|37|03.7}} | style="background: {{star-color|M}};" | M4 V | 0.27 | 10.95 | 12.45 | has two disputed planets |
| rowspan='3' | Omicron2 Eridani (40 Eridani, Gliese 166) | style="background-color: lightgreen" | Keid (A){{Dollar sign}} | rowspan="3" |16.3330 | rowspan='3' |Eri |{{RA|04|15|16.3}} |
| 07|39|10}}
| style="background: {{star-color|K}};" | K0.5 V | 0.84 | style="background: lightblue;" | 4.43{{Hash-tag|alt=visible to naked eye}} | 5.93 | rowspan="3" |199.6911 | has one refuted planet |
| style="background: #F5F5DC" | B{{Double-dagger|alt=white dwarf}}
| {{RA|04|15|21.8}} | style="background: #F5F5DC" | DA4 | 0.573 | 9.52 | 11.02 | |
| C
| {{RA|04|15|21.5}} | style="background: {{star-color|M}};" | M4 V | 0.2036 | 11.24 | 12.74 | |
| colspan = '2' | EV Lacertae
| 16.4761 | style="background-color: pink" | Lac{{Asterisk}} | {{RA|22|46|49.7}} | style="background: {{star-color|M}};" | M3.5 V | 0.35 | 10.22 | 11.70 | record setting stellar flare observed |
| rowspan='2' | 70 Ophiuchi (Gliese 702)
| style="background-color: lightgreen" | A{{Dollar sign}} | rowspan='2' | 16.7074 | rowspan='2' | Oph | {{RA|18|05|27.4}} | style="background: {{star-color|K}};" | K0 V | 0.90 | style="background: lightblue;" | 4.21{{Hash-tag|alt=visible to naked eye}} | 5.66 | rowspan='2' | 195.2166 | rowspan="2" | |
| style="background-color: lightgreen" | B{{Dollar sign}}
| {{RA|18|05|27.5}} | style="background: {{star-color|K}};" | K5 V | 0.70 | style="background: lightblue;" | 6.01{{Hash-tag|alt=visible to naked eye}} | 7.46 |
| colspan = '2' style="background-color: lightgreen" | Altair (Alpha Aquilae){{Dollar sign}}
| 16.730 | style="background-color: pink" | Aql{{Asterisk}} | {{RA|19|50|47.0}} | style="background: {{star-color|A}}" | A7 IV-Vn | 1.79 | style="background: lightblue;" | 0.77{{Hash-tag|alt=visible to naked eye}} | 2.22 | |
| rowspan='2' | EI Cancri (GJ 1116, {{nowrap|G 9-38}})
| A | rowspan='2' | 16.800 | rowspan='2' | Cnc | rowspan='2' | {{RA|08|58|15.2}} | style="background: {{star-color|M}};" | M5.5 V | 0.12 | 14.06 | 15.50 | rowspan='2' | 194.1443 | rowspan="2" | |
| B
| style="background: {{star-color|M}};" | M V | 0.10 | 14.92 | 16.36 |
| colspan = '2' style="background: #D8BD98" | WISE J150649.97+702736.1§
| 16.856 | style="background-color: pink" | UMi{{Asterisk}} | {{RA|15|06|52.4}} | style="background: {{star-color|T}};" | T6 | | 13.74 J | 15.17 J | |
| colspan = '2' | GJ 3379 ({{nowrap|G 99-49}})
| 16.9861 | style="background-color: pink" | Ori{{Asterisk}} | {{RA|06|00|03.5}} | style="background: {{star-color|M}};" | M3.5 V | 0.2312 | 11.31 | 12.73 | |
| colspan = '2' style="background: #D8BD98" | DENIS J081730.0−615520§
| 17.002 | Car | {{RA|08|17|30.1}} | style="background: {{star-color|T}};" | T6 | 0.015 | 13.61 J | 15.03 J | |
| colspan = '2' | Gliese 445 (LHS 2459, {{nowrap|G 254-29}})
| 17.1368 | style="background-color: pink" | Cam{{Asterisk}} | {{RA|11|47|41.4}} | style="background: {{star-color|M}};" | M3.5 V | 0.14 | 10.79 | 12.19 | |
| colspan = '2' | 2MASS J15404342−5101357
| 17.3738 | style="background-color: pink" | Nor{{Asterisk}} | {{RA|15|40|43.5}} |
| 51|01|36}}
| style="background: {{star-color|M}};" | M7 V | 0.090 | 15.26 | 16.63 | |
| rowspan='2' | 2MASS 0939−2448
| style="background: #D8BD98" | A§ | rowspan='2' | 17.41 | rowspan='2' | Ant | rowspan='2' | {{RA|09|39|35.5}} | style="background: {{star-color|T}};" | T8 V | 0.019–0.048 | 15.61 J | 16.97 J | rowspan='2' | 187.3 | rowspan='2' | binary brown dwarf |
| style="background: #D8BD98" | B§
| style="background: {{star-color|T}};" | T8 V | 0.019–0.038 | | |
| colspan = '2' | GJ 3323 (LHS 1723, {{nowrap|LP 656-38}})
| 17.5309 | Eri | {{RA|05|01|57.4}} | style="background: {{star-color|M}};" | M4 V | 0.1705 | 12.22 | 13.57 | has two known planets |
| colspan = '2' | Gliese 526 (Wolf 498, HD 119850)
|17.7263 | style="background-color: pink" | Boo{{Asterisk}} | {{RA|13|45|43.8}} | style="background: {{star-color|M}};" | M1 V | 0.28 | 8.46 | 9.78 | |
| colspan = '2' style="background: #D8BD98" | WISE 0350−5658§
| 17.84 | style="background-color: pink" | Ret{{Asterisk}} | {{RA|03|50|00.3}} |
| 56|58|30}}
| style="background: {{star-color|Y}};" | Y1 | | 22.47 J | 23.70 J | |
| rowspan='2' | Stein 2051 (Gliese 169.1, {{nowrap|G 175-34}})
| A | rowspan='2' | 17.9925 | rowspan='2' | Cam | {{RA|04|31|11.5}} | style="background: {{star-color|M}};" | M4 V | 0.252 | 11.04 | 12.33 | rowspan='2' | 181.2730 | rowspan="2" | |
| style="background: #F5F5DC" | B{{Double-dagger|alt=white dwarf}}
| {{RA|04|31|12.6}} | style="background: #F5F5DC" | DC5 | 0.675 | 12.43 | 13.72 |
| colspan = '2' style="background: #D8BD98" | 2MASS J11145133−2618235§
| 18.20 | Hya | {{RA|11|14|51.3}} | style="background: {{star-color|T}};" | T7.5 | 0.029–0.048 | 15.86 J | 17.12 J | 179.2 | |
| colspan = '2' | Gliese 251 (Wolf 294, HD 265866)
| 18.2146 | style="background-color: pink" | Gem{{Asterisk}} | {{RA|06|54|49.0}} | style="background: {{star-color|M}};" | M3 V | 0.360 | 10.02 | 11.29 | has one known planet |
| colspan = '2' | LP 816-60
| 18.3305 | style="background-color: pink" | Cap{{Asterisk}} | {{RA|20|52|33.0}} |
| 16|58|29}}
| style="background: {{star-color|M}};" | M3.5 V | 0.224 | 11.50 | 12.75 | |
| colspan = '2' | LSR J1835+3259
| 18.5534 | style="background-color: pink" | Lyr{{Asterisk}} | {{RA|18|35|37.9}} | style="background: {{star-color|M}};" | M8.5 V | 0.053 | 18.27 | 19.50 | |
| colspan = '2' | Gliese 205 (Wolf 1453, HD 36395)
| 18.6042 | Ori | {{RA|05|31|27.4}} | style="background: {{star-color|M}};" | M1 V | 0.556 | 7.95 | 9.17 | |
| colspan = '2' style="background: #D8BD98" | 2MASS J04151954−0935066§
| 18.62 | Eri | {{RA|04|15|19.5}} | style="background: {{star-color|T}};" | T8 | 0.03 | 15.34 J | 16.56 J | |
| rowspan='3' | Gliese 229 (HD 42581)
| A | rowspan='3' | 18.7906 | rowspan='3' style="background-color: pink" | Lep{{Asterisk}} | rowspan='3' | {{RA|06|10|34.6}} | style="background: {{star-color|M}};" | M1.5 V | 0.579 | 8.14 | 9.34 |
| style="background: #D8BD98" | Ba§
| style="background: {{star-color|T}};" | T7 | 0.036 | rowspan=2 | 14.01 J | rowspan=2 | 15.21 J |
| style="background: #D8BD98" | Bb§
| style="background: {{star-color|T}};" | T8 | 0.033 |
| colspan = '2' style="background-color: lightgreen" | Alsafi (Sigma Draconis){{Dollar sign}}
| 18.7993 | Dra | {{RA|19|32|21.6}} | style="background: {{star-color|G}};" | G9 V | 0.85 | style="background: lightblue;" | 4.67{{Hash-tag|alt=visible to naked eye}} | 5.87 | |
| colspan = '2' | Ross 47 (Gliese 213)
| 18.8883 | Ori | {{RA|05|42|09.3}} | style="background: {{star-color|M}};" | M4 V | 0.35 | 11.57 | 12.76 | |
| colspan = '2' style="background: #D8BD98" | WISE 1541−2250§
| 18.93 | Lib | {{RA|15|41|51.6}} | style="background: {{star-color|Y}};" | Y0.5 | 0.011 | 20.99 J | 22.10 J | |
| rowspan='4' | Gliese 570 (Lalande 27173, 33 G. Librae) | style="background-color: lightgreen" | A{{Dollar sign}} | rowspan='4' | 19.1987 | rowspan='4' style="background-color: pink" | Lib{{Asterisk}} | rowspan='4' | {{RA|14|57|28.0}} |
| 21|24|56}}
| style="background: {{star-color|K}};" | K4 V | 0.802 | style="background: lightblue;" | 5.64{{Hash-tag|alt=visible to naked eye}} | 6.79 | rowspan='4' | 169.8843 | rowspan='4' | |
| B
| style="background: {{star-color|M}};" | M1.5 V | 0.55 | 8.30 | 9.45 |
| C
| style="background: {{star-color|M}};" | M | 0.35 | 9.96 | 11.11 |
| style="background: #D8BD98" | D§
| style="background: {{star-color|T}};" | T7.5 | 0.05 | 15.32 J | 16.47 J |
| colspan = '2' | Gliese 693 (Luyten 205–128)
| 19.2078 | Pav | {{RA|17|46|32.4}} |
| 57|19|09}}
| style="background: {{star-color|M}};" | M3 V | 0.26 | 10.76 | 11.91 | |
| colspan = '2' | Gliese 754 (Luyten 347–14)
| 19.2724 | style="background-color: pink" | Tel{{Asterisk}} | {{RA|19|20|48.0}} | style="background: {{star-color|M}};" | M4 V | 0.173 | 12.23 | 13.37 | has one candidate planet |
| colspan = '2' | Gliese 908 (Lalande 46650, BR Piscium)
| 19.2745 | Psc | {{RA|23|49|12.5}} | style="background: {{star-color|M}};" | M1 V | 0.37 | 8.98 | 10.12 | |
| rowspan='2' | Gliese 752 (Wolf 1055, HD 180617)
| A | rowspan='2' | 19.2922 | rowspan='2' | Aql | {{RA|19|16|55.3}} | style="background: {{star-color|M}};" | M2.5 V | 0.46 | 9.10 | 10.24 | rowspan='2' | 169.0615 | has one known planet |
| B {{Nowrap|(VB 10)}}
| {{RA|19|16|57.6}} | style="background: {{star-color|M}};" | M8 V | 0.075 | 17.45 | 18.59 | very small and very dim red dwarf |
| colspan = '2' | Gliese 588 (CD-40 9712)
| 19.2996 | style="background-color: pink" | Lup{{Asterisk}} | {{RA|15|32|12.9}} |
| 41|16|32}}
| style="background: {{star-color|M}};" | M2.5 V | 0.43 | 9.31 | 10.45 | has two candidate planets |
| rowspan='2' | Eta Cassiopeiae (Gliese 34)
| style="background-color: lightgreen" | Achird (A){{Dollar sign}} | rowspan='2' | 19.3314 | rowspan='2' style="background-color: pink" | Cas{{Asterisk}} | rowspan='2' | {{RA|00|49|06.3}} | style="background: {{star-color|G}};" | G3 V | 0.972 | style="background: lightblue;" | 3.46{{Hash-tag|alt=visible to naked eye}} | 4.60 | rowspan='2' | 168.7186 | rowspan="2" | |
| B
| style="background: {{star-color|K}};" | K7 V | 0.57 | 7.51 | 8.65 |
| rowspan='3' | 36 Ophiuchi (Gliese 663)
| style="background-color: lightgreen" | Guniibuu (A){{Dollar sign}} | rowspan='3' | 19.4185 | rowspan='3' | Oph | {{RA|17|15|20.9}} |
| 26|36|09}}
| style="background: {{star-color|K}};" | K1.5 V | 0.85 | style="background: lightblue;" | 5.07{{Hash-tag|alt=visible to naked eye}} | 6.20 | rowspan='3' | 167.9617 | rowspan='3' | |
| style="background-color: lightgreen" | B{{Dollar sign}}
| {{RA|17|15|21.0}} |
| 26|36|10}}
| style="background: {{star-color|K}};" | K1 V | 0.85 | style="background: lightblue;" | 5.08{{Hash-tag|alt=visible to naked eye}} | 6.21 |
| style="background-color: lightgreen" | C{{Dollar sign}}
| {{RA|17|16|13.4}} |
| 26|32|46}}
| style="background: {{star-color|K}};" | K5 V | 0.71 | style="background: lightblue;" | 6.32{{Hash-tag|alt=visible to naked eye}} | 7.45 |
| colspan = '2' | YZ Canis Minoris (Ross 882, Gliese 285)
| 19.5330 | CMi | {{RA|07|44|40.2}} | style="background: {{star-color|M}};" | M4 V | 0.308 | 11.19 | 12.30 | |
| rowspan='2' | GJ 1005 ({{nowrap|Luyten 722-22}}, {{nowrap|G 158-50}})
| A | rowspan="2" | 19.577 | rowspan="2" | Cet | rowspan="2" | {{RA|00|15|28.1}} |
| 16|08|02}}
| style="background: {{star-color|M}};" | M3.5 V | 0.179 | 11.60 | 12.71 | rowspan="2" | distance uncertain: 16.28±0.75, 17.91±0.67, 17.0±1.5, 16.26±0.76, 17.26, 19.695±0.095 ly{{Citation needed|date=March 2025}} |
| B
| style="background: {{star-color|M}};" | M V | 0.112 | 14.02 | 15.13 |
| rowspan='2' | HR 7703 (279 G. Sagittarii, HD 191408, Gliese 783, {{nowrap|IRAS 20079-3614}})
| style="background-color: lightgreen" | A{{Dollar sign}} | rowspan='2' | 19.609 | rowspan='2' | Sgr | rowspan='2' | {{RA|20|11|11.93}} | style="background: {{star-color|K}};" | K2.5 V | 0.65 | style="background: lightblue;" | 5.31{{Hash-tag|alt=visible to naked eye}} | 6.41 | rowspan='2' | 166.3272 | rowspan='2' | |
| B
| style="background: {{star-color|M}};" | M4 V | 0.24 | 11.50 | 12.60 |
| colspan = '2' style="background-color: lightgreen" | 82 G. Eridani (e Eridani, Gliese 139, HD 20794){{Dollar sign}}
| 19.7045 | Eri | {{RA|03|19|55.7}} | style="background: {{star-color|G}};" | G8 V | 0.70 | style="background: lightblue;" | 4.26{{Hash-tag|alt=visible to naked eye}} | 5.35 |has three confirmed planets, three candidate planets, hot and cold dust disks |
| rowspan='2' | Gliese 268 (Ross 986, QY Aurigae)
| A | rowspan='2' | 19.7414 | rowspan='2' style="background-color: pink" | Aur{{Asterisk}} | rowspan='2' | {{RA|07|10|01.8}} | style="background: {{star-color|M}};" | M4.5 V | 0.226 | 12.05 | 13.14 | rowspan='2' | 165.2147 | rowspan='2' | |
| B
| style="background: {{star-color|M}};" | M V | 0.192 | 12.45 | 13.54 |
| colspan = '2' style="background-color: lightgreen" | Delta Pavonis{{Dollar sign}}
| 19.893 | Pav | {{RA|20|08|43.6}} | style="background: {{star-color|G}};" | G8 IV | 1.051 | style="background: lightblue;" | 3.55{{Hash-tag|alt=visible to naked eye}} | 4.62 | has one candidate planet |
| colspan = '2' style="background: #D8BD98" | SIMP J013656.5+093347§
| 19.955 | Psc | {{RA|01|36|56.5}} | style="background: {{star-color|T}};" | T2.5 | 0.012 | 13.25 J | 14.32 J | rogue planet, 12.7 MJ |
| colspan = '2' style="background: #D8BD98" | 2MASS 0937+2931§
| 19.96 | Leo | {{RA|09|37|34.9}} | style="background: {{star-color|T}};" | T7 | 0.040 | 14.65 J | 15.71 J | 163.39 | |
| class="unsortable"
!Star or (sub-) brown dwarf ! rowspan="2" |Distance ! rowspan="2" | ! rowspan="2" |Coordinates: ! rowspan="2" |Stellar ! rowspan="2" |Mass ! data-sort-type="number" |App. ! data-sort-type="number" |Abs. ! rowspan="2" |Parallax ! rowspan="2" |Notes and additional |
| class="unsortable"
! colspan="2" |Designation |
Distant future and past encounters
File:Sun_in_orbit_around_Galactic_Centre.gif (yellow dot and white curve) around the Galactic Centre (GC) in the last galactic year. The red dots correspond to the positions of the stars studied by the European Southern Observatory in a monitoring programme.{{cite web|title=Milky Way Past Was More Turbulent Than Previously Known | url= http://www.eso.org/public/news/eso0411/ |work=ESO News|publisher = European Southern Observatory |date = 2004-04-06 |quote= After more than 1,000 nights of observations spread over 15 years, they have determined the spatial motions of more than 14,000 solar-like stars residing in the neighbourhood of the Sun.}}]]
Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astrometric measurements of parallax and total proper motions, along with spectroscopically determined radial velocities. Although extrapolations can be made into the past or future, they are subject to increasingly significant cumulative errors over very long periods. Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.See also: Stellar kinematics.
One of the first stars known to approach the Sun particularly close is Gliese 710. The star, whose mass is roughly half that of the Sun, is currently 62 light-years from the Solar System. It was first noticed in 1999 using data from the Hipparcos satellite, and was estimated to pass less than {{Convert|1.3|ly|pc}} from the Sun in 1.4 million years.{{cite journal |last1=García-Sánchez |first1=Joan |last2=Preston |first2=Robert A. |last3=Jones |first3=Dayton L. |last4=Weissman |first4=Paul R. |last5=Lestrade |first5=Jean-François |last6=Latham |first6=David W. |last7=Stefanik |first7=Robert P. |title=Stellar Encounters with the Oort Cloud Based on Hipparcos Data |journal=The Astronomical Journal |date=February 1999 |volume=117 |issue=2 |pages=1042–1055 |doi=10.1086/300723 |bibcode=1999AJ....117.1042G |s2cid=122929693 |doi-access=free }} With the release of Gaia's observations of the star, it has since been refined to a much closer {{convert|0.178|ly|pc}}, close enough to significantly disturb objects in the Oort cloud, which extends {{convert|1.2|ly|pc}} from the Sun.{{cite journal |last1=Bailer-Jones |first1=C. A. L. |last2=Rybizki |first2=J. |last3=Andrae |first3=R. |last4=Fouesneau |first4=M. |title=New stellar encounters discovered in the second data release |journal=Astronomy & Astrophysics |date=13 August 2018 |volume=616 |pages=A37 |doi=10.1051/0004-6361/201833456 |arxiv=1805.07581 |bibcode=2018A&A...616A..37B |s2cid=56269929 }}
Gaia{{'s}} third data release has provided updated values for many of the candidates in the table below.{{cite journal | last1=Bailer-Jones | first1=C. A. L. | date=13 July 2022 | title=Stars that approach within one parsec of the Sun: New and more accurate encounters identified in Gaia Data Release 3 | journal=The Astrophysical Journal Letters | volume= 935| issue= 1| page= 152| arxiv=2207.06258 | bibcode=2022ApJ...935L...9B | doi=10.3847/2515-5172/ac842b | s2cid=251154282 | url= | doi-access=free }}{{cite journal | last1=Bobylev | first1=Vadim | last2=Bajkova | first2=Anisa | date=14 July 2022 | title=Search for Close Stellar Encounters with the Solar System Based on Data from the Gaia DR3 Catalogue | journal=Astronomy Letters | volume=48 | issue=9 | pages=542–549 | doi=10.1134/S1063773722080011 | arxiv=2206.14443| bibcode=2022AstL...48..542B | s2cid=256832377 }}{{cite journal |last1=de la Fuente Marcos |first1=Raúl
|last2=de la Fuente Marcos |first2=Carlos |date=28 June 2022 |title=An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced |journal=Research Notes of the AAS |volume= 6 |issue= 6 |pages= 136 |arxiv=
|bibcode=2022RNAAS...6..136D |doi= 10.3847/2515-5172/ac7b95|doi-access=free }}{{cite journal | last1=de la Fuente Marcos | first1=Carlos | last2=de la Fuente Marcos | first2=Raúl | date=28 July 2022 | title=The Closest Past Flyby of a Known Star to the Solar System: HD 7977, UCAC4 237-008148 or WISE J072003.20-084651.2? | journal=Research Notes of the AAS | volume=6 | issue=7 | pages=152 | arxiv= | bibcode=2022RNAAS...6..152D | doi=10.3847/2515-5172/ac842b | s2cid=251154282 | doi-access=free }}
| class="wikitable sortable sticky-header-multi" style="text-align:center"
|+Stars that are known to have passed or will pass within 5 light-years of the Sun in the past or futureTable 3, {{cite journal |last=Bobylev |first=Vadim V. | date=March 2010 |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B|s2cid=118374161 }}{{cite journal|title=New stellar encounters discovered in the second Gaia data release|journal=Astronomy & Astrophysics|volume=616|issue=37|pages=A37|last1=Bailer-Jones|first1=C. A. L.|last2=Rybizki|first2=J.|last3=Andrae|first3=R.|last4=Fouesneau|first4=M.|date=19 May 2018|arxiv=1805.07581|doi=10.1051/0004-6361/201833456|bibcode=2018A&A...616A..37B|s2cid=56269929 }}{{cite journal |last1=Bobylev |first1=Vadim |last2=Bajkova |first2=Anisa |title=Search for Close Stellar Encounters with the Solar System Based on Data from the Gaia DR3 Catalogue |journal=Astronomy Letters |date=29 June 2022 |volume=48 |issue=9 |pages=542–549 |doi=10.1134/S1063773722080011 |arxiv=2206.14443 |bibcode=2022AstL...48..542B |s2cid=256832377 }} ! Star name ! Minimum distance ! Date of approach ! Current distance ! Mass in M☉ ! Current ! Current Constellation ! Current ! Current |
| Gliese 710
| {{val|0.167|0.012}} | {{val|1296|24|23}} | {{val|62.248|0.020}} | K7V | 0.4–0.6 | {{sort|09.6|9.6}} | Serpens | {{RA|18|19|50.843}} | {{DEC|−01|56|18.98}} |
| HD 7977
| {{val|0.478|0.104|0.078}} | {{val |
| 2764|28|29}}
| {{val|246.74|0.60}} | G0V | ~1.2 | {{sort|09.04|9.04}} | {{RA|01|20|31.597}} | {{DEC|+61|52|57.08}} |
|
| Scholz's Star and companion brown dwarf | {{val|0.82|0.37|0.22}} | {{val |
| 78.5|0.7}}
| {{val|22.2|0.2}} | A: M9V | A: 0.095 | {{sort|18.3|18.3}} | {{RA|07|20|03.20}} | {{DEC |
| 08|46|51.2}} |
| 2MASS J0628+1845
| {{val|1.61|0.28|0.24}} | {{val|1720|150|130}} | {{val|272.28|0.80}} | M2.5V | 0.28 | {{sort|16.2|16.2}} | Gemini | {{RA|06|28|11.593}} | {{DEC|+18|45|12.91}} |
| 2MASS J0805+4624
| {{val|1.610|0.099|0.092}} | {{val |
| 363|13|14}}
| {{val|238.1|1.0}} | M3V | 0.25 | {{sort|17.0|17.0}} | Lynx | {{RA|08|05|29.038}} | {{DEC|+46|24|51.78}} |
| CD-69 2001
| {{val|1.616|0.070|0.068}} | {{val |
| 1907|10}}
| {{val|332.61|0.55}} | K4V | 0.61 | {{sort|11.13|11.13}} | Indus | {{RA|21|40|31.514}} | {{DEC |
| 69|25|14.58}} |
| HD 49995
| {{val|1.70|0.23|0.20}} | {{val |
| 4034|94|98}}
| {{val|439.74|0.59}} | A: F3V | A: 1.48 | 8.78 | {{RA|06|50|20.810}} | {{DEC |
| 18|37|30.58}} |
| 2MASS J0621-0101
| {{val|1.71|0.46|0.39}} | {{val |
| 3206|68|66}}
| {{val|428.8|3.1}} | G5V | 0.96 | 11.9 | Orion | {{RA|06|21|34.807}} | {{DEC |
| 01|01|55.01}} |
|
| {{val|1.8557|0.0048}} | {{val|84.59|0.19}} | {{val|22.9858|0.0034}} | M5V | ~0.15 | {{sort|10.82|10.82}} | Cygnus | {{RA|21|46|22.285}} | {{DEC|+38|13|03.12}} |
| 2MASS J0455+1144
| {{val|1.94|0.16|0.15}} | {{val|1702|58|54}} | {{val|349.50|0.80}} | M0V | 0.50 | {{sort|15.3|15.3}} | Orion | {{RA|04|55|21.427}} | {{DEC|+11|44|41.25}} |
| 2MASS J0734-0637
| {{val|1.950|0.021}} | {{val |
| 554.6|3.3}}
| {{val|130.66|0.12}} | M0V | 0.50 | {{sort|12.9|12.9}} | {{RA|07|34|39.097}} | {{DEC |
| 06|37|12.21}} |
| 2MASS J1151-0313
| {{val|1.98|0.20|0.18}} | {{val|1017|60|54}} | {{val|125.88|0.41}} | M3.5V | 0.23 | {{sort|15.3|15.3}} | Virgo | {{RA|11|51|37.434}} | {{DEC |
| 03|13|45.24}} |
| UCAC4 076–006432
| {{val|2.042|0.034|0.033}} | {{val |
| 893.8|7.9|8.0}}
| {{val|212.41|0.15}} | mid K | ~0.6 | {{sort|12.69|12.69}} | Mensa | {{RA|06|34|29.385}} | {{DEC |
| 74|49|47.12}} |
|
| {{val|2.25|0.17|0.15}} | {{val|473|27|25}} | {{val|237.56|0.66}} | M3.5V | 0.25 | {{sort|16.5|16.5}} | {{RA|01|20|04.561}} | {{DEC|+47|39|46.56}} |
| TYC 6760–1510–1
| {{val|2.46|0.19|0.18}} | {{val |
| 1708|44|47}}
| {{val|102.89|0.16}} | M1.5V | 0.58 | {{sort|11.5|11.5}} | Hydra | {{RA|15|00|09.536}} | {{DEC |
| 29|05|27.67}} |
| UCAC2 15719371
| {{val|2.46|0.10}} | {{val |
| 4282|70|73}}
| {{val|280.80|0.26}} | K4V | 0.66 | {{sort|12.58|12.58}} | Antlia | {{RA|09|44|09.884}} | {{DEC |
| 37|45|31.09}} |
|
| {{val|2.637|0.055|0.054}} | {{val |
| 1536.6|9.0|9.1}}
| {{val|286.51|0.40}} | Early K | ~0.8 | {{sort|10.95|10.95}} | {{RA|21|14|32.911}} | {{DEC|+21|53|32.76}} |
| HD 179939
| {{val|2.65|0.17}} | {{val|3020|25}} | {{val|334.32|0.88}} | A3V | 1.7 | {{sort|07.23|7.23}} | Aquila | {{RA|19|14|10.043}} | {{DEC|+07|45|50.72}} |
| BD-21 1529
| {{val|2.701|0.059|0.058}} | {{val |
| 1660.1|6.3}}
| {{val|368.48|0.56}} | G5V | ~0.95 | {{sort|09.67|9.67}} | {{RA|06|37|48.004}} | {{DEC |
| 21|22|21.94}} |
| 2MASS J1310-1307
| {{val|2.79|0.59|0.47}} | {{val |
| 1520|150|190}}
| {{val|433.0|2.6}} | M2.5V | 0.34 | {{sort|16.3|16.3}} | Virgo | {{RA|13|10|30.804}} | {{DEC |
| 13|07|33.55}} |
| UPM J1121-5549
| {{val|2.803|0.020}} | {{val |
| 282.5|1.6|1.7}}
| {{val|72.498|0.029}} | M3V | 0.29 | {{sort|13.5|13.5}} | {{RA|11|21|18.136}} | {{DEC |
| 55|49|17.77}} |
| UCAC4 464–006057
| {{val|2.812|0.052|0.051}} | {{val|932|11}} | {{val|101.570|0.086}} | Early M | ~0.4 | {{sort|11.73|11.73}} | Taurus | {{RA|04|09|02.050}} | {{DEC|+02|45|38.32}} |
|
| {{val|2.91|0.13|0.12}} | {{val |
| 306|12|13}}
| {{val|80.987|0.048}} | M5.0 | 0.17 | {{sort|16.4|16.4}} | Puppis | {{RA|06|21|54.714}} | {{DEC |
| 47|25|31.33}} |
| GJ 3649
| {{val|3.016|0.024}} | {{val |
| 520.4|3.1}}
| {{val|54.435|0.023}} | M1 | 0.49 | {{sort|10.85|10.85}} | Leo | {{RA|11|12|38.97}} | {{DEC|+18|56|05.4}} |
| Ross 248
| {{val|3.0446|0.0077}} | {{val|38.500|0.096}} | {{val|10.3057|0.0014}} | M6V | 0.136 | {{sort|12.29|12.29}} | {{RA|23|41|54.99}} | {{DEC|+44|10|40.8}} |
| 2MASS J1921-1244
| {{val|3.08|0.21|0.19}} | {{val |
| 3490|120|130}}
| {{val|376.46|0.73}} | K6V | 0.69 | {{sort|12.46|12.46}} | {{RA|19|21|58.124}} | {{DEC |
| 12|43|58.61}} |
| Proxima Centauri
| {{val|3.123|0.015}} | {{val|28.65|0.27}} | {{val|4.24646|0.00028}} | M5Ve | 0.15 | {{sort|11.05|11.05}} | {{RA|14|29|42.949}} | {{DEC|−62|40|46.14}} |
| TYC 9387–2515–1
| {{val|3.220|0.081|0.079}} | {{val |
| 1509.1|8.6|8.7}}
| {{val|401.96|0.54}} | K1V | 0.86 | {{sort|11.45|11.45}} | Mensa | {{RA|06|18|54.643}} | {{DEC |
| 80|19|16.54}} |
| Alpha Centauri AB
| {{val|3.242|0.060}} | {{val|29.63|1.00|0.98}} | {{val|4.321|0.024}} | A: G2V | A: 1.100 | A: -0.01 | {{RA|14|39|36.495}} | {{DEC|−60|50|02.31}} |
| Gliese 445
| {{val|3.3400|0.0051}} | {{val|46.341|0.065}} | {{val|17.1368|0.0017}} | M4 | 0.15? | {{sort|10.8|10.8}} | {{RA|11|47|41.377}} | {{DEC|+78|41|28.18}} |
| 2MASS J1638-6355
| {{val|3.37|0.29|0.28}} | {{val |
| 1428|21|22}}
| {{val|468.5|4.2}} | K2V | 0.82 | {{sort|12.44|12.44}} | {{RA|16|38|21.759}} | {{DEC |
| 63|55|13.16}} |
| 2MASS J0542+3217
| {{val|3.43|0.75|0.71}} | {{val|5823|89|87}} | {{val|884.6|2.4}} | A: G4V | A: 1.01 | {{sort|12.80|12.80}} | Auriga | {{RA|05|42|38.349}} | {{DEC|+32|17|29.85}} |
| 2MASS J0625-2408
| {{val|3.700|0.082|0.080}} | {{val |
| 1874|14}}
| {{val|534.88|0.93}} | K/M | ~0.5 | {{sort|12.91|12.91}} | {{RA|06|25|42.744}} | {{DEC |
| 24|08|35.02}} |
| Barnard's Star
| {{val|3.7682|0.0031}} | {{val|11.735|0.013}} | {{val|5.96290|0.00044}} | sdM4 | 0.144 | {{sort|09.54|9.54}} | {{RA|17|57|48.498}} | {{DEC|+04|41|36.25}} |
| BD+05 1792
| {{val|3.965|0.040}} | {{val |
| 962.7|3.0}}
| {{val|239.73|0.33}} | G2V | 1.07 | {{sort|08.58|8.58}} | Gemini | {{RA|07|48|07.037}} | {{DEC|+05|27|22.51}} |
| 2MASS J2241-2759
| {{val|4.05|0.16}} | {{val |
| 2810|37|38}}
| {{val|411.06|0.76}} | K7V | ~0.5 | {{sort|12.28|12.28}} | {{RA|22|41|50.996}} | {{DEC |
| 27|59|47.04}} |
| 2MASS J1724-0522
| {{val|4.15|0.26|0.25}} | {{val|3058|54|52}} | {{val|489.5|1.3}} | K0V | 0.86 | {{sort|12.73|12.73}} | {{RA|17|24|55.056}} | {{DEC |
| 05|22|11.45}} |
| StKM 1–554
| {{val|4.217|0.036|0.035}} | {{val |
| 549.9|2.9|3.0}}
| {{val|151.97|0.19}} | M0V | 0.65 | {{sort|12.17|12.17}} | Orion | {{RA|05|14|01.871}} | {{DEC|+05|22|56.26}} |
| GJ 3379
| {{val|4.227|0.024}} | {{val |
| 157.43|0.93|0.94}}
| {{val|16.9861|0.0027}} | M3.5V | 0.19 | {{sort|11.31|11.31}} | Orion | {{RA|06|00|03.824}} | {{DEC|+02|42|22.97}} |
| 2MASS J1936+3627
| {{val|4.23|0.62|0.57}} | {{val|3830|120|110}} | {{val|671.6|3.4}} | G5.5V | 0.95 | 12.2 | Cygnus | {{RA|19|36|57.294}} | {{DEC|+36|27|57.71}} |
| 2MASS J0710+5228
| {{val|4.303|0.039}} | {{val|507.6|3.8|3.7}} | {{val|90.949|0.050}} | M3V | 0.33 | {{sort|12.52|12.52}} | Lynx | {{RA|07|10|52.167}} | {{DEC|+52|28|18.49}} |
| HD 146248
| {{val|4.341|0.040|0.039}} | {{val |
| 1141.5|3.7}}
| {{val|334.87|0.47}} | G2/3IV | 1.23 | {{sort|09.47|9.47}} | {{RA|16|19|27.875}} | {{DEC |
| 64|50|34.38}} |
| 2MASS J1724+0355
| {{val|4.37|0.12}} | {{val|1991|38|37}} | {{val|254.99|0.26}} | G8V | 0.85 | {{sort|12.54|12.54}} | {{RA|17|24|34.633}} | {{DEC|+03|55|26.75}} |
| StKM 1–1456
| {{val|4.396|0.043}} | {{val|1240.2|6.9|6.8}} | {{val|144.934|0.095}} | A: K5V | A: 0.81 | {{sort|10.58|10.58}} | Hercules | {{RA|17|17|31.118}} | {{DEC|+15|34|55.35}} |
| Zeta Leporis
| {{val|4.43|0.33|0.30}} | {{val |
| 878|42|46}}
| {{val|72.81|0.40}} | A2Vann | 2.0 | {{sort|03.55|3.55}} | Lepus | {{RA|05|46|57.341}} | {{DEC|−14|49|19.02}} |
| Lalande 21185
| {{val|4.6807|0.0055}} | {{val|21.973|0.033}} | {{val|8.30437|0.00068}} | M2V | 0.39 | {{sort|07.52|7.52}} | {{RA|11|03|20.194}} | {{DEC|+35|58|11.55}} |
| HD 68814
| {{val|4.724|0.090|0.089}} | {{val |
| 2242|13}}
| {{val|259.85|0.30}} | G6V | 0.98 | {{sort|09.57|9.57}} | Hydra | {{RA|08|13|57.112}} | {{DEC |
| 04|03|12.56}} |
| 2MASS J1941-4602
| {{val|4.814|0.050|0.049}} | {{val |
| 456.5|4.1|4.2}}
| {{val|66.848|0.033}} | M4-M6 | ~0.15 | {{sort|12.4|12.4}} | {{RA|19|41|53.18}} | {{DEC |
| 46|02|31.4}} |
{{wide image|Objects_between_sun_and_alpha_centauri.jpg|2500px|
Schematic view to scale of past and future close approaches of stars to the Sun (Up to 4.5 light-years)}}
See also
{{col div|colwidth=30em}}
- Interstellar travel
- Location of Earth
- The Magnificent Seven
- Nearby Stars Database
- Solar System#Galactic context
- Stars in fiction
{{colend}}
=Related lists=
{{col div|colwidth=30em}}
- List of stars with resolved images
- List of brightest stars
- List of star systems within 20–25 light-years
- List of star systems within 25–30 light-years
- List of star systems within 30–35 light-years
- List of star systems within 35–40 light-years
- List of star systems within 40–45 light-years
- List of star systems within 45–50 light-years
- List of star systems within 50–55 light-years
- List of star systems within 55–60 light-years
- List of star systems within 60–65 light-years
- List of star systems within 65–70 light-years
- List of star systems within 70–75 light-years
- List of star systems within 75–80 light-years
- List of star systems within 80–85 light-years
- List of star systems within 85–90 light-years
- List of star systems within 90–95 light-years
- List of star systems within 95–100 light-years
- List of nearest giant stars
- List of nearest supergiants
- List of nearest bright stars
- Historical brightest stars
- List of nearest exoplanets
- List of nearest terrestrial exoplanet candidates
- List of nearest stars by spectral type
- List of nearby stellar associations and moving groups
- List of star-forming regions in the Local Group
- Lists of stars
- List of Solar System objects by greatest aphelion
- List of trans-Neptunian objects
- List of nearest known black holes
{{colend}}
Notes
{{reflist |group=note}}
References
External links
- [http://www.astro.gsu.edu/RECONS/TOP100.posted.htm "The 100 nearest star systems"], Research Consortium on Nearby Stars
- {{cite web
|title = NStars database
|website = Northern Arizona University
|url = http://nstars.nau.edu
|access-date = 2005-10-24
|url-status = dead
|archive-url = https://web.archive.org/web/20051030160049/http://nstars.nau.edu/
|archive-date = October 30, 2005
|df = mdy-all
}}
- {{Cite APOD
|title=Map of the 25 nearest star systems
|date=March 18, 2001
|access-date=2005-10-24}}
- {{cite web
|title=Notable Nearby Stars
|website=SolStation
|url=http://www.solstation.com/stars.htm
|access-date=2005-10-24}}
- {{cite web
|title=Cool stars in the solar Neighbourhood
|website=D. Montes, UCM
|url=http://www.ucm.es/info/Astrof/invest/actividad/cool_NS.html
|access-date=2005-11-14}}
- [http://adsabs.harvard.edu/abs/1994QJRAS..35....1M The dynamics of the closest stars]
- {{cite web
|author=Takeda, G.
|author2=E. B. Ford |author3=A. Sills |author4=F. A. Rasio |author5=D. A. Fischer |author6=J. A. Valenti
|date=2006
|url=http://exoplanets.org/SPOCS_evol.html
|title=Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~ 1000 Cool Stars from the SPOCS Catalog
|publisher=California & Carnegie Planet Search
|access-date=2006-10-13
}}
- [http://www.bodurov.com/NearestStars/ Nearest Stars 3D View]
- Table 4 "The Census of Stars and Brown Dwarfs within 8 Parsecs of the Sun" in {{Cite journal |arxiv=1205.2122|last1=Bailer-Jones|first1=C. A. L.|display-authors=etal|title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function|journal=The Astrophysical Journal|volume=753|issue=2|pages=156|year=2012|doi=10.1088/0004-637X/753/2/156|bibcode=2012ApJ...753..156K|s2cid=119279752}}
{{star}}
{{Nearest star systems}}
{{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar System}}
nearest stars and brown dwarfs
nearest stars and brown dwarfs