82 G. Eridani#Planetary system

{{about-distinguish|e Eridani|epsilon Eridani{{!}}ε Eridani}}

{{Starbox image

| image=

{{Location mark

| image=Eridanus constellation map.svg

| float=center | width=250 | position=right

| mark=Red circle.svg | mark_width=5 | mark_link=82 Eri

| x%=59.3 | y%=70.1

}}

| caption=Location of 82 G. Eridani (circled)

}}

{{Starbox observe

| epoch=J2000

| constell=Eridanus

| ra={{RA|03|19|55.651}}

| dec={{DEC|−43|04|11.22}}

| appmag_v=4.254

}}

{{Starbox character

| type = main sequence

| class=G6 V

| b-v=+0.71

| u-b=+0.22

| variable=

}}

{{Starbox astrometry

| radial_v={{val|87.76|0.13}}

| prop_mo_ra=3,035.017

| prop_mo_dec=726.964

| pm_footnote=

| parallax=165.5242

| p_error=0.0784

| parallax_footnote=

| absmag_v=5.34

}}

{{Starbox detail

| source =

| mass={{val|0.79|0.01}}

| radius={{val|0.93|0.03}}

| luminosity={{val|0.6869|0.0026}}

| habitable_inner={{val|0.6322|0.0020|ul=AU}}

| habitable_outer={{val|1.5236|0.0091|ul=AU}}

| gravity={{val|4.39|0.03}}

| temperature={{val|5473|48|fmt=commas}}

| metal_fe={{val|−0.42|0.02}}

| rotation=~39 days

| rotational_velocity=<2

| age_gyr={{val|5.76|0.66}}, 11.3

}}

{{Starbox catalog

| names={{odlist | B=e Eri, e Eridani | G=82 G. Eridani, 82 G. Eri | HD=20794 | CD=−43°1028 | GCTP=703 | GJ=139 | LHS=19 | LTT=1583 | HR=1008 | SAO=216263 | FK5=119 | HIP=15510 }}

}}

{{Starbox reference

| Simbad = LHS+19 | sn=The star

| Simbad2 = GJ+139+b | sn2=planet b

| Simbad3 = GJ+139+c | sn3=planet c

| Simbad4 = GJ+139+d | sn4=planet d

| NSTED = HD20794

| ARICNS = 00297

| EPE = HD+20794

}}

82 G. Eridani (HD 20794, Gliese 139, e Eridani) is a star {{convert|19.7|ly|pc|lk=on|abbr=off}} away from Earth in the constellation Eridanus. It is a main-sequence star with a stellar classification of G6 V, and it hosts a system of three confirmed planets and a dust disk.

Observation

In the southern-sky catalog Uranometria Argentina, 82 G. Eridani (often abbreviated to 82 Eridani) is the 82nd star listed in the constellation Eridanus. The Argentina catalog, compiled by the 19th-century astronomer Benjamin Gould, is a southern celestial hemisphere analog of the more famous Flamsteed catalog, and uses a similar numbering scheme. 82 G. Eridani, like other stars near the Sun, has held on to its Gould designation, even while other more distant stars have not.{{cn|date=January 2023}}

Properties

82 G. Eridani is slightly smaller and less massive than the Sun, at around 80% of the Sun's mass and 90% of the radius. It has a luminosity 30% fainter than the Sun's. Spectroscopically, it is classified as G6V, compared to G2V for the Sun, and is among the nearest solar-type stars. The projected rotational velocity rate (v sin i) is smaller than 2 km/s, compatible with a slow-rotating or pole-on star relative to Earth. Such observation would also match the lack of a reliable rotational period detection and the absence of any magnetic cycle.

It is a high-velocity star—it is moving quickly compared to the average—and hence is probably a member of Population II, generally older stars whose motions take them well outside the plane of the Milky Way. Like many other Population II stars, 82 G. Eridani is somewhat metal-deficient (though much less deficient than many), and is older than the Sun. It has a relatively high orbital eccentricity of 0.42 about the galaxy, ranging between 3.52 and 8.41 kiloparsecs from the core. Its age is estimated at 5.76 billion years, based on its chromospheric activity indicator, but other estimates suggest ages close or higher to the age of the Universe.

This star is located in a region of low-density interstellar matter (ISM), so it is believed to have a large astropause that subtends an angle of 6″ across the sky. Relative to the Sun, this star is moving at a space velocity of 101 km/s, with the bow shock advancing at more than Mach 3 through the ISM.

Planetary system

An infrared excess was discovered around the star by the Infrared Space Observatory at 60 μm, but was not later confirmed by the Spitzer Space Telescope, in 2006. However, in 2012, a dust disk was found around the star, by the Herschel Space Observatory. While not well-constrained, if assumed to have a similar composition to 61 Virginis' dust disk, it has a semi-major axis of 24 AU.

On August 17, 2011, European astronomers announced the discovery of three planets orbiting 82 G. Eridani. The mass range of these planets classifies them as super-Earths; objects with only a few times the Earth's mass. These planets were discovered by precise measurements of the radial velocity of the star, with the planets revealing their presence by their gravitational displacement of the star during each orbit. None of the planets display a significant orbital eccentricity. However, their orbital periods are all 90 days or less, indicating that they are orbiting close to the host star. The equilibrium temperature for the most distant planet, based on an assumed Bond albedo of 0.3, would be about {{Convert|388|K|C}}; significantly above the boiling point of water.

At the time of planet c's detection, it exerted the lowest gravitational perturbation. There was also a similarity noted between its orbital period and the rotational period of the star. For these reasons the discovery team were somewhat more cautious regarding the verity of its candidate planet status than for the other two. (Indeed this 40-day planet is no longer believed to exist and the "c" designation has been re-used.)

Using the TERRA algorithm, developed by Guillem Anglada-Escudé and R. Paul Butler in 2012, to describe better and filter out noise interference to extract more precise radial velocity measurements, a team of scientists led by Fabo Feng, in 2017, provided evidence for up to three more planets. One such candidate, of Neptune mass, 82 G. Eridani f, may orbit in the habitable zone of the star. The team also believe that, using these noise reduction techniques, they are able to better quantify the descriptions for the earlier 3 exoplanets, but only have weak evidence of 82 G. Eridani c.

A study in 2023 could only confirm planets b & d, and did not significantly detect the other planet candidates. In particular, the statistical significance of planet c would be expected to increase with additional data; the fact that this has not happened casts doubt on its existence. The 40-day radial velocity signal may instead be tied to the stellar rotation. The additional three candidates found in 2017 (e, f, g) could not be confirmed or refuted.{{rp|23,44}} Another 2023 study also only confirmed b & d out of the previous planet candidates (referring to them as b & c), but also detected a potential third planet farther from the star than any of the previous candidates, on an eccentric orbit partially within the habitable zone. A 2024 study confirmed this habitable zone planet.

{{Orbitbox planet begin

| name = 82 Eridani

| table_ref = {{efn|The Cretignier et al. 2023 and Nari et al. 2025 references used here refer to the 90-day planet as "c" and the new 640-day planet as "d". Previous publications refer to the 90-day planet as "d", with "c" referring to a 40-day candidate that is likely a false positive. Additional candidates found by Feng et al. 2017 are not included here as they are not detected by more recent studies.}}

}}

{{OrbitboxPlanet disk

| disk = Hot dust

| periapsis =

| apoapsis = ≲0.1

}}

{{Orbitbox planet

| exoplanet = b

| mass_earth = {{val|2.15|0.17|p=≥}}

| semimajor = {{val|0.12570|0.00052|0.00053}}

| period = {{val|18.3140|0.0022}}

| eccentricity = {{val|0.064|0.065|0.046}}

}}

{{Orbitbox planet

| exoplanet = c

| mass_earth = {{val|2.98|0.29|p=≥}}

| semimajor = {{val|0.3625|0.0015|0.0016}}

| period = {{val|89.68|0.10}}

| eccentricity = {{val|0.077|0.084|0.055}}

}}

{{Orbitbox planet

| exoplanet = d

| mass_earth = {{val|5.82|0.57|p=≥}}

| semimajor = {{val|1.3541|0.0068}}

| period = {{val|647.6|2.5|2.7}}

| eccentricity = {{val|0.45|0.11|0.10}}

}}

{{OrbitboxPlanet disk

| disk = Dust disk

| periapsis = 22

| apoapsis = 27

| inclination = 50

}}

=Potential habitability of HD 20794 d=

On October 15, 2024, researchers at Oxford University announced that they had confirmed HD 20794 d, orbiting in the habitable zone of its star. In an article published in the journal Astronomy & Astrophysics, scientists said an analysis of 20 years of observational data had found HD 20794 d could be a rocky planet (though its composition is unknown and it could also be a mini-Neptune{{rp|10}}) and should be "a high-priority target for future atmospheric characterization with direct imaging facilities."

About six times the mass of Earth, the planet orbits "at the right distance from its star to sustain liquid water on its surface — a key ingredient for life as we know it." However, HD 20794 d's orbit is significantly elliptical, meaning it spends part of its year outside the habitable zone. Data for the research was gathered at the High Accuracy Radial Velocity Planet Searcher spectrograph at La Silla Observatory in Chile. With the discovery, HD 20794 d became the 12th-closest potentially habitable planet to Earth.

Planned observation missions

82 G. Eridani (GJ 139) was picked as a Tier 1 target star for NASA's proposed Space Interferometry Mission (SIM) mission to search for terrestrial-sized or larger planets, which was cancelled in 2010.

Notes

{{Notelist|notes=

}}

References

{{reflist|1=30em|refs=

{{Cite journal |last=Luck |first=R. Earle |date=2018-03-01 |title=Abundances in the Local Region. III. Southern F, G, and K Dwarfs |bibcode=2018AJ....155..111L |journal=The Astronomical Journal |volume=155 |issue=3 |pages=111 |doi=10.3847/1538-3881/aaa9b5 |doi-access=free |issn=0004-6256}}

{{cite journal|bibcode=2004yCat.4027....0K|title=VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)|journal=VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002)|volume=4027|last1=Kostjuk|first1=N. D.|year=2004}}

{{cite journal |bibcode= 2002yCat.2237....0D |title= VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system |last1= Ducati |first1= J. R. |journal= Vizier Online Data Catalog |date= 2002 |volume= 2237 }}

{{cite web | url=http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+20794&submit=SIMBAD+search | title=LHS 19 -- High proper-motion Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | access-date=2007-07-26}}

{{cite book | first1=Benjamin Apthorp | last1=Gould | title=Uranometria Argentina: brightness and position of every fixed star, down to the seventh magnitude, within one hundred degrees of the South Pole | volume=1 | series=Resultados, Universidad Nacional de Córdoba Observatorio Astronómico | publisher=Observatorio Nacional Argentino | date=1879 | pages=159–160 | url=https://books.google.com/books?id=VhE1AQAAIAAJ&pg=PA159}} Coordinates are for the 1875 equinox.

{{Cite journal |last1=Bernkopf |first1=J. |last2=Chini |first2=R. |last3=Buda |first3=L. -S. |last4=Dembsky |first4=T. |last5=Drass |first5=H. |last6=Fuhrmann |first6=K. |last7=Lemke |first7=R. |date=2012-09-01 |title=Characteristics of the closest known G-type exoplanet host 82 Eri |bibcode=2012MNRAS.425.1308B |journal=Monthly Notices of the Royal Astronomical Society |volume=425 |issue=2 |pages=1308–1311 |doi=10.1111/j.1365-2966.2012.21534.x |doi-access=free |issn=0035-8711}}

{{cite journal | last=Hearnshaw | first=J. B. | title=The iron abundance of 82 Eridani | journal=Astronomy and Astrophysics | date=1973 | volume=29 | pages=165–170 | bibcode=1973A&A....29..165H}}

{{cite journal | bibcode=1989ApJS...71..245K | title=The Perkins Catalog of Revised MK Types for the Cooler Stars | journal=The Astrophysical Journal Supplement Series | volume=71 | pages=245 | last1=Keenan | first1=Philip C | last2=McNeil | first2=Raymond C | year=1989 | doi=10.1086/191373}}

{{cite journal | last=Frisch | first=P. C. | title=G-star astropauses - A test for interstellar pressure | journal=Astrophysical Journal | date=1993 | volume=407 | issue=1 | pages=198–206 | bibcode=1993ApJ...407..198F | doi=10.1086/172505}}

{{cite journal | last1=Holmberg | first1=J. | last2=Nordstrom | first2=B. | last3=Andersen | first3=J. | title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics | journal=Astronomy and Astrophysics | volume=501 | issue=3 |date=July 2009 | pages=941–947 | doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H|arxiv = 0811.3982 | s2cid=118577511}}

{{cite web | first=Chris | last=McCarthy | date=2005 | url=http://tauceti.sfsu.edu/~chris/SIM/ | title=SIM Planet Search Tier 1 Target Stars | publisher=San Francisco State University | access-date=2007-07-26 | archive-url=https://web.archive.org/web/20070810132311/http://tauceti.sfsu.edu/~chris/SIM/ | archive-date=2007-08-10 | url-status=dead}}

{{cite journal | display-authors=1 | last1=Pepe | first1=F. | last2=Lovis | first2=C. | last3=Ségransan | first3=D. | last4=Benz | first4=W. | last5=Bouchy | first5=F. | last6=Dumusque | first6=X. | last7=Mayor | first7=M. | last8=Queloz | first8=M. | last9=Queloz | first9=D. | last10=Udry | first10=S. |title=The HARPS search for Earth-like planets in the habitable zone: I – Very low-mass planets around HD20794, HD85512 and HD192310 | journal=Astronomy & Astrophysics | volume=534 | pages=A58 | date=2011 | arxiv=1108.3447 | bibcode=2011A&A...534A..58P | doi=10.1051/0004-6361/201117055 | s2cid=15088852}}

{{cite news |last1=Burgess |first1=Kaya |title=‘Super-Earth’ discovered — and it’s a prime candidate for alien life |url=https://www.thetimes.com/uk/science/article/super-earth-discovered-and-its-a-prime-candidate-for-alien-life-jw0z60vfw |access-date=28 January 2025 |work=The Times of London |date=28 January 2025 |language=en}}{{cite news |title=Researchers confirm the existence of an exoplanet in the habitable zone {{!}} University of Oxford |url=https://www.ox.ac.uk/news/2025-01-28-researchers-confirm-existence-exoplanet-habitable-zone |access-date=28 January 2025 |work=www.ox.ac.uk |date=28 January 2025 |language=en}}

{{Cite journal | doi = 10.1093/mnras/stv511| title = Kuiper belt structure around nearby super-Earth host stars| journal = Monthly Notices of the Royal Astronomical Society| volume = 449| issue = 3| pages = 3121| year = 2015| last1 = Kennedy | first1 = G. M.| last2 = Matra | first2 = L.| last3 = Marmier | first3 = M.| last4 = Greaves | first4 = J. S.| last5 = Wyatt | first5 = M. C.| last6 = Bryden | first6 = G.| last7 = Holland | first7 = W.| last8 = Lovis | first8 = C.| last9 = Matthews | first9 = B. C.| last10 = Pepe | first10 = F.| last11 = Sibthorpe | first11 = B.| last12 = Udry | first12 = S.| doi-access = free|arxiv = 1503.02073 |bibcode = 2015MNRAS.449.3121K | s2cid = 53638901}}

{{cite journal | last1=Feng |first1=F. |last2=Tuomi |first2=M. |last3=Jones |first3=H.R.A.|date=September 2017 | journal=Astronomy and Astrophysics |title = Evidence for at least three planet candidates orbiting HD 20794 |volume=605 |issue=103 |arxiv = 1705.05124 | doi=10.1051/0004-6361/201730406 |bibcode=2017A&A...605A.103F |pages=11 |s2cid=119084078}}

{{cite journal | display-authors=1 |last1=Wyatt |first1=M. C. |last2=Kennedy |first2=G. |last3=Sibthorpe |first3=B. |last4=Moro-Martín |first4=A. |last5=Lestrade |first5=J.-F. |last6=Ivison |first6=R. J. |last7=Matthews |first7=B. |last8=Udry |first8=S. |last9=Greaves |first9=J. S. |last10=Kalas |first10=P. |last11=Lawler |first11=S. |last12=Su |first12=K. Y. L. |last13=Rieke |first13=G. H. |last14=Booth |first14=M. |last15=Bryden |first15=G. |last16=Horner |first16=J. |last17=Kavelaars |first17=J. J. |last18=Wilner |first18=D. |date = 2012 | journal=Monthly Notices of the Royal Astronomical Society |volume=424 |issue=2 |pages=1206 |title = Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems |arxiv = 1206.2370 | doi=10.1111/j.1365-2966.2012.21298.x |doi-access=free |bibcode = 2012MNRAS.424.1206W |s2cid=54056835}}

{{cite journal | display-authors=1 |last1=Decin |first1=G. |last2=Dominik |first2=C. |last3=Malfait |first3=K. |last4=Mayor |first4=M. |last5=Waelkens |first5=C.|date=May 2000 | journal=Astronomy and Astrophysics |title = The Vega phenomenon around G dwarfs |volume=357 |bibcode=2000A&A...357..533D |pages=533–542}}

{{cite journal |last1=Laliotis |first1=Katherine |last2=Burt |first2=Jennifer A. |display-authors=etal |date=April 2023 |title=Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions |journal=The Astronomical Journal |volume=165 |issue=4 |pages=176 |doi=10.3847/1538-3881/acc067 |arxiv=2302.10310 |bibcode=2023AJ....165..176L |doi-access=free}}

{{cite journal |last1=Cretignier |first1=M. |last2=Dumusque |first2=X. |display-authors=etal |date=August 2023 |title=YARARA V2: Reaching sub-m s⁻¹ precision over a decade using PCA on line-by-line radial velocities |journal=Astronomy & Astrophysics |volume=678 |pages=A2 |doi=10.1051/0004-6361/202347232 |arxiv=2308.11812 |bibcode=2023A&A...678A...2C |s2cid=261076243}}

{{cite journal |last1=Nari |first1=N. |last2=Dumusque |first2=X. |last3=Hara |first3=N. C. |last4=Suárez Mascareño |first4=A. |last5=Cretignier |first5=M. |last6=González Hernández |first6=J. I. |last7=Stefanov |first7=A. K. |last8=Passegger |first8=V. M. |last9=Rebolo |first9=R. |last10=Pepe |first10=F. |last11=Santos |first11=N. C. |last12=Cristiani |first12=S. |last13=Faria |first13=J. P. |last14=Figueira |first14=P. |last15=Sozzetti |first15=A. |last16=Zapatero Osorio |first16=M. R. |last17=Adibekyan |first17=V. |last18=Alibert |first18=Y. |last19=Allende Prieto |first19=C. |last20=Bouchy |first20=F. |last21=Benatti |first21=S. |last22=Castro-González |first22=A. |last23=D’Odorico |first23=V. |last24=Damasso |first24=M. |last25=Delisle |first25=J. B. |last26=Di Marcantonio |first26=P. |last27=Ehrenreich |first27=D. |last28=Génova-Santos |first28=R. |last29=Hobson |first29=M. J. |last30=Lavie |first30=B. |last31=Lillo-Box |first31=J. |last32=Lo Curto |first32=G. |last33=Lovis |first33=C. |last34=Martins |first34=C. J. a. P. |last35=Mehner |first35=A. |last36=Micela |first36=G. |last37=Molaro |first37=P. |last38=Mordasini |first38=C. |last39=Nunes |first39=N. |last40=Palle |first40=E. |last41=Quanz |first41=S. P. |last42=Ségransan |first42=D. |last43=Silva |first43=A. M. |last44=Sousa |first44=S. G. |last45=Udry |first45=S. |last46=Unger |first46=N. |last47=Venturini |first47=J. |display-authors=2 |date=28 January 2025 |title=Revisiting the multi-planetary system of the nearby star HD 20794. Confirmation of a low-mass planet in the habitable zone of a nearby G-dwarf |journal=Astronomy & Astrophysics |volume=693 |issue= |pages=A297 |doi=10.1051/0004-6361/202451769 |doi-access=free |language=en |issn=0004-6361 |arxiv=2501.17092}}

}}