82 G. Eridani
Location of 82 G. Eridani (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension 03h 19m 55.651s[1]
Declination −43° 04′ 11.22″[1]
Apparent magnitude (V) 4.254[2]
Characteristics
Spectral type G6 V[3]
U−B color index +0.22[4]
B−V color index +0.71[4]
Astrometry
Radial velocity (Rv)87.76±0.13[1] km/s
Proper motion (μ) RA: 3035.017 mas/yr[1]
Dec.: 726.964 mas/yr[1]
Parallax (π)165.5242 ± 0.0784 mas[1]
Distance19.704 ± 0.009 ly
(6.041 ± 0.003 pc)
Absolute magnitude (MV)5.34[2]
Details
Mass0.70[5] M☉
Radius0.92[6] R☉
Luminosity0.74[7] L☉
Surface gravity (log g)4.40[8] cgs
Temperature5,401[8] K
Metallicity [Fe/H]−0.40[8] dex
Rotation33.19 ± 3.61 days[5]
Rotational velocity (v sin i)4.0[9] km/s
Age6.1[10]–12.7[2] Gyr
Other designations
e Eri, e Eridani, CD−43°1028, FK5 119, GJ 139, HD 20794, HIP 15510, HR 1008, SAO 216263, G 82 G. Eridani, 82 G. Eri, LHS 19, LTT 1583[4]
Database references
SIMBADThe star
planet b
planet c
planet d
Exoplanet Archivedata
ARICNSdata

82 G. Eridani (HD 20794, HR 1008, e Eridani) is a star 19.7 light-years (6.0 parsecs) 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 at least three planets and a dust disk.

Observation

In the southern-sky catalog Uranometria Argentina, 82 G. Eridani (often abbreviated to 82 Eridani)[11] is the 82nd star listed in the constellation Eridanus.[12] 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.

Properties

This star is slightly smaller and less massive than the Sun, making it marginally dimmer than the Sun in terms of luminosity; it is about a third more luminous than Tau Ceti or Alpha Centauri B. The projected equatorial rotation rate (v sin i) is 4.0 km/s,[9] compared to 2 km/s for the Sun. However, this value is likely overestimated and explained by the limitation of the spectrograph used. When observed by HARPS, a v sin i smaller than 2 km/s is found, compatible with a slow-rotating or inclined star. Such observation would also match the lack of a reliable rotational period detection and the absence of any magnetic cycle.[13]

82 G. Eridani 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 0.40 about the galaxy, ranging between 4.6 and 10.8 kiloparsecs from the core. Estimates of the age of this star ranged from 6 to 12 billion years.[10][14]

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.[15]

Planetary system

An infrared excess was discovered around the star by the Infrared Space Observatory at 60 μm,[16] but was not later confirmed by the Spitzer Space Telescope, in 2006. However, in 2012, a dust disk was found around the star,[17] 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 19 AU.[18]

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 388 K (115 °C); significantly above the boiling point of water.[5]

The number of planets in the system remains uncertain. 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.[5] Continued observation of the star will be required to determine the exact nature of the planetary system.

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.[19]

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.[20]: 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.[13]

The 82 Eridani (2017) planetary system[18][19]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
Hot dust ≲0.1 AU — —
g (unconfirmed) ≥1.03+0.49
−0.30 M⊕		 0.095 ± 0.001 11.86+0.01
−0.02		 0.20+0.15
−0.19		 — —
b ≥2.82+0.10
−0.80 M🜨		 0.127 ± 0.001 18.33+0.01
−0.02		 0.27+0.04
−0.22		 — —
c (unconfirmed) ≥2.52+0.52
−0.83 M⊕		 0.225+0.002
−0.003		 43.17+0.12
−0.10		 0.17+0.10
−0.16		 — —
d ≥3.52+0.58
−1.01 M🜨		 0.364 ± 0.004 88.90+0.37
−0.41		 0.25+0.16
−0.21		 — —
e ≥4.77+0.96
−0.86 M🜨		 0.509 ± 0.006 147.02+1.43
−0.91		 0.29+0.14
−0.18		 — —
f (unconfirmed) ≥10.26+1.89
−1.47 M⊕		 0.875 ± 0.001 331.41+5.08
−3.01		 0.05+0.06
−0.05		 — —
Dust disk ~19–~30 AU — —
The 82 Eridani (2023) planetary system[18][13]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
Hot dust ≲0.1 AU — —
b ≥2.0±0.2 M🜨 0.13±0.01 18.32±0.01 0.09+0.08
−0.06		 — —
c ≥4.7±0.4 M🜨 0.37±0.01 89.58+0.09
−0.10		 0.13±0.07 — —
d (unconfirmed) ≥6.6+0.6
−0.7 M⊕		 1.36±0.03 644.6+9.9
−7.7		 0.40±0.07 — —
Dust disk ~19–~30 AU — —

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,[21] which was cancelled in 2010.

See also

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511
  3. ↑ Keenan, Philip C; McNeil, Raymond C (1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. 1 2 3 "LHS 19 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2007-07-26
  5. 1 2 3 4 Pepe, F.; et al. (2011), "The HARPS search for Earth-like planets in the habitable zone: I – Very low-mass planets around HD20794, HD85512 and HD192310", Astronomy & Astrophysics, 534: A58, arXiv:1108.3447, Bibcode:2011A&A...534A..58P, doi:10.1051/0004-6361/201117055, S2CID 15088852
  6. ↑ Johnson, H. M.; Wright, C. D. (1983), "Predicted infrared brightness of stars within 25 parsecs of the sun", Astrophysical Journal Supplement Series, 53: 643–711, Bibcode:1983ApJS...53..643J, doi:10.1086/190905 — See the table on p. 653.
  7. ↑ Porto de Mello, Gustavo; del Peloso, Eduardo F.; Ghezzi, Luan (April 2006), "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun", Astrobiology, 6 (2): 308–331, arXiv:astro-ph/0511180, Bibcode:2006AsBio...6..308P, doi:10.1089/ast.2006.6.308, PMID 16689649, S2CID 119459291
  8. 1 2 3 Sousa, S. G.; et al. (August 2007), "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes", Astronomy and Astrophysics, 487 (1): 373–381, arXiv:0805.4826, Bibcode:2008A&A...487..373S, doi:10.1051/0004-6361:200809698, S2CID 18173201
  9. 1 2 Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377
  10. 1 2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID 27151456
  11. ↑ Kostjuk, N. D. (2004). "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)". VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002). 4027. Bibcode:2004yCat.4027....0K.
  12. ↑ Gould, Benjamin Apthorp (1879), Uranometria Argentina: brightness and position of every fixed star, down to the seventh magnitude, within one hundred degrees of the South Pole, Resultados, Universidad Nacional de Córdoba Observatorio Astronómico, vol. 1, Observatorio Nacional Argentino, pp. 159–160 Coordinates are for the 1875 equinox.
  13. 1 2 3 Cretignier, M.; Dumusque, X.; et al. (August 2023). "YARARA V2: Reaching sub-m s−1 precision over a decade using PCA on line-by-line radial velocities". Astronomy & Astrophysics. 678: A2. arXiv:2308.11812. Bibcode:2023A&A...678A...2C. doi:10.1051/0004-6361/202347232. S2CID 261076243.
  14. ↑ Hearnshaw, J. B. (1973), "The iron abundance of 82 Eridani", Astronomy and Astrophysics, 29: 165–170, Bibcode:1973A&A....29..165H
  15. ↑ Frisch, P. C. (1993), "G-star astropauses - A test for interstellar pressure", Astrophysical Journal, 407 (1): 198–206, Bibcode:1993ApJ...407..198F, doi:10.1086/172505
  16. ↑ Decin, G.; et al. (May 2000). "The Vega phenomenon around G dwarfs". Astronomy and Astrophysics. 357: 533–542. Bibcode:2000A&A...357..533D.
  17. ↑ Wyatt, M. C.; et al. (2012). "Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems". Monthly Notices of the Royal Astronomical Society. 424 (2): 1206. arXiv:1206.2370. Bibcode:2012MNRAS.424.1206W. doi:10.1111/j.1365-2966.2012.21298.x. S2CID 54056835.
  18. 1 2 3 Kennedy, G. M.; Matra, L.; Marmier, M.; Greaves, J. S.; Wyatt, M. C.; Bryden, G.; Holland, W.; Lovis, C.; Matthews, B. C.; Pepe, F.; Sibthorpe, B.; Udry, S. (2015). "Kuiper belt structure around nearby super-Earth host stars". Monthly Notices of the Royal Astronomical Society. 449 (3): 3121. arXiv:1503.02073. Bibcode:2015MNRAS.449.3121K. doi:10.1093/mnras/stv511. S2CID 53638901.
  19. 1 2 Feng, F.; Tuomi, M.; Jones, H.R.A. (September 2017). "Evidence for at least three planet candidates orbiting HD 20794". Astronomy and Astrophysics. 605 (103): 11. arXiv:1705.05124. Bibcode:2017A&A...605A.103F. doi:10.1051/0004-6361/201730406. S2CID 119084078.
  20. ↑ Laliotis, Katherine; Burt, Jennifer A.; et al. (April 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal. 165 (4): 176. arXiv:2302.10310. Bibcode:2023AJ....165..176L. doi:10.3847/1538-3881/acc067.
  21. ↑ McCarthy, Chris (2005). "SIM Planet Search Tier 1 Target Stars". San Francisco State University. Archived from the original on 2007-08-10. Retrieved 2007-07-26.
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