Epsilon Eridani b

Epsilon Eridani b / AEgir
An artist's impression of Epsilon Eridani b, depicting it as a gas giant with rings. The object near the bottom is a hypothetical moon.
Discovery[1]
Discovered byHatzes et al.
Discovery siteUnited States
Discovery date7 August 2000
Doppler spectroscopy
Orbital characteristics[2]
3.53±0.06 AU
Eccentricity0.26±0.04
2,688.60+16.17
−16.51 d
7.36+0.04
−0.05 yr
Inclination130.60°+9.53°
−12.62°
206.07°+15.14°
−17.48°
2444411.54+76.60
−81.95 JD
166.48°+6.63°
−6.66°
Semi-amplitude9.98+0.43
−0.38 m/s
StarEpsilon Eridani
Physical characteristics
Mass0.76+0.14
−0.11 MJ[2]
Temperature~150 K (−123 °C; −190 °F)[3]

Epsilon Eridani b, also known as AEgir [sic],[4] is an exoplanet approximately 10.5 light-years away orbiting the star Epsilon Eridani, in the constellation of Eridanus (the River). The planet was discovered in 2000, and as of 2024 remains the only confirmed planet in its planetary system. It orbits at around 3.5 AU with a period of around 7.6 years, and has a mass around 0.6 times that of Jupiter.[5] As of 2023, both the Extrasolar Planets Encyclopaedia and the NASA Exoplanet Archive list the planet as 'confirmed'.[6][7]

Name

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The planet and its host star are one of the planetary systems selected by the International Astronomical Union as part of NameExoWorlds, their public process for giving proper names to exoplanets and their host star (where no proper name already exists).[8][9] The process involved public nomination and voting for the new names.[10] In December 2015, the IAU announced the winning names were AEgir [sic] for the planet (pronounced /ˈiːdʒər/ [Anglicized] or /ˈeɪjɪər/, an approximation of the old Norse Ægir) and Ran for the star.[11] James Ott, age 14, submitted the names for the IAU contest and won.[12]

The moon Aegir of Saturn is also named after the mythological Ægir, and differs in spelling only by capitalization.[13]

Discovery

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The planet's existence was suspected by a Canadian team led by Bruce Campbell and Gordon Walker in the early 1990s, but their observations were not definitive enough to make a solid discovery. Its formal discovery was announced on August 7, 2000, by a team led by Artie Hatzes. The discoverers gave its mass as 1.2 ± 0.33 times that of Jupiter, with a mean distance of 3.4 AU from the star.[1] Observers, including Geoffrey Marcy, suggested that more information on the star's Doppler noise behaviour created by its large and varying magnetic field was needed before the planet could be confirmed.[14]

In 2006, the Hubble Space Telescope made astrometric measurements and confirmed the existence of the planet.[15] These observations indicated that the planet has a mass 1.5 times that of Jupiter and shares the same plane as the outer dust disk observed around the star.[16] The derived orbit from these measurements is eccentric: either 0.25[16] or 0.7.[17]

Meanwhile, the Spitzer Space Telescope detected an asteroid belt at roughly 3 AU from the star.[18] In 2009 one team of astronomers claimed that the proposed planet's eccentricity and this belt were inconsistent: the planet would pass through the asteroid belt and rapidly clear it of material.[19] The planet and the inner belt may be reconciled if that belt's material had migrated in from the outer comet belt (also known to exist).[20]

Astronomers continue to collect and analyse radial velocity data, while also refining existing upper limits from non-detection via direct imaging, on Epsilon Eridani b. A paper published in January 2019 found an orbital eccentricity with an order of magnitude smaller than earlier estimates had, at around 0.07, consistent with a nearly circular orbit and very similar to Jupiter's orbital eccentricity of 0.05.[3] This resolved the stability issue with the inner asteroid belt. The updated measurements, amongst other things, also included new estimates for the mass and inclination of the planet, at 0.78 times that of Jupiter but due to the inclination having been poorly constrained at 89 degrees this was only a rough estimate of the absolute mass.[3] If the planet instead orbited at the same inclination as the debris disc (34 degrees), as supported by Benedict et al. 2006,[16] then its mass would have been greater, at 1.19 times that of Jupiter.[3]

Using astrometric data taken from the U.S. Naval Observatory Robotic Astrometric Telescope (URAT) combined with previously collected data from the Hipparcos mission, and the newer Gaia EDR3 data release, a group of scientists at the United States Naval Observatory believe they have, with high formal confidence levels, confirmed the presence of a long-period exoplanet orbiting Epsilon Eridani.[21]

A paper published in October 2021 determines, using absolute astrometry measurements from the Hipparcos, Gaia DR2 data, and new radial velocity measurements from Keck/NIRC2 Ms-band vortex coronagraph images, a lower absolute mass of 0.65 times that of Jupiter, at an eccentricity close to 0.055 with the planet orbiting at around 3.53 AU inclined at 78 degrees.[22][23][nb 1] Similar updated findings were published in a paper in July 2021, determining a minimum mass of 0.651 that of Jupiter, with the planet's semi-major axis at 3.5 AU orbiting with an eccentricity of 0.044.[7][24] A March 2022 paper finds an inclination of 45 degrees, closer to earlier estimates, a mass 0.63 times that of Jupiter, and an eccentricity of 0.16.[5]

Direct imaging of Epsilon Eridani b with the James Webb Space Telescope is planned.[25]

See also

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Notes

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  1. ^ The eccentricity figure is quoted from table 3 in the Llop-Sayson et al 2021 paper,[23] calculated from radial velocity measurements alone and without an assumption of age. If astrometric measurements and direct imaging are also taken into account, as in table 4, with an age of 800 million years assumed for Epsilon Eridani, then the absolute mass is 0.66+0.12
    −0.09     MJ     and it is orbiting with an eccentricity of 0.07+0.08
    −0.05    .

References

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  1. ^ a b Hatzes, Artie P.; et al. (2000). "Evidence for a Long-Period Planet Orbiting ε Eridani". The Astrophysical Journal. 544 (2): L145–L148. arXiv:astro-ph/0009423. Bibcode:2000ApJ...544L.145H. doi:10.1086/317319. S2CID 117865372.
  2. ^ a b Feng, Fabo; Butler, R. Paul; et al. (July 2023). "Revised orbits of the two nearest Jupiters". Monthly Notices of the Royal Astronomical Society. 525 (1): 607–619. arXiv:2307.13622. Bibcode:2023MNRAS.525..607F. doi:10.1093/mnras/stad2297.
  3. ^ a b c d Mawet, Dimitri; Hirsch, Lea; et al. (2019). "Deep Exploration of ϵ Eridani with Keck Ms-band Vortex Coronagraphy and Radial Velocities: Mass and Orbital Parameters of the Giant Exoplanet" (PDF). The Astronomical Journal. 157 (1): 33. arXiv:1810.03794. Bibcode:2019AJ....157...33M. doi:10.3847/1538-3881/aaef8a. ISSN 1538-3881. OCLC 7964711337. S2CID 119350738.
  4. ^ Carroll, Michael (2017), "Zeroing in on Earth 2.0", Earths of Distant Suns, Springer, p. 79, doi:10.1007/978-3-319-43964-8_5, ISBN 978-3-319-43963-1, Planet name: AEgir | Original designation: Epsilon Eridani b
  5. ^ a b Benedict, G. Fritz (March 2022). "Revisiting HST/FGS Astrometry of epsilon Eridani". Research Notes of the AAS. 6 (3): 45. Bibcode:2022RNAAS...6...45B. doi:10.3847/2515-5172/ac5b6b.
  6. ^ "Planet eps Eridani b". Extrasolar Planets Encyclopaedia. Retrieved 5 July 2021. Planet Status: Confirmed
  7. ^ a b "eps Eri Overview". NASA Exoplanet Archive. NASA Exoplanet Science Institute. Retrieved 5 October 2021. Status: Confirmed Planet
  8. ^ "NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars". IAU.org. 9 July 2014. Retrieved 2017-09-25.
  9. ^ "The ExoWorlds". nameexoworlds.iau.org: IAU. Archived from the original on 2016-12-31. Retrieved 2017-09-25.
  10. ^ "NameExoWorlds". nameexoworlds.iau.org: IAU. Retrieved 2017-09-25.
  11. ^ "Final Results of NameExoWorlds Public Vote Released". International Astronomical Union. 15 December 2015. Retrieved 2017-09-25.
  12. ^ "Mountainside wins competition to name planet, star". Spokesman.com. Retrieved 2016-05-12.
  13. ^ "Planetary Names". planetarynames.wr.usgs.gov. Retrieved 6 January 2023.
  14. ^ Marcy, Geoffrey W.; et al. (August 7–11, 2000). "Planetary Messages in the Doppler Residuals (Invited Review)". In A. Penny (ed.). Planetary Systems in the Universe, Proceedings of IAU Symposium #202. Manchester, United Kingdom. p. 20–28. Bibcode:2004IAUS..202...20M.
  15. ^ "Hubble Zeroes in on Nearest Known Exoplanet". Hubble News Desk. 2006-10-09. Retrieved 2006-10-10.
  16. ^ a b c Benedict, G. Fritz; et al. (2006). "The Extrasolar Planet ε Eridani b: Orbit and Mass". The Astronomical Journal. 132 (5): 2206–2218. arXiv:astro-ph/0610247. Bibcode:2006AJ....132.2206B. doi:10.1086/508323. S2CID 18603036. Retrieved 2008-11-16.
  17. ^ Butler; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
  18. ^ Backman, D.; et al. (2009). "Epsilon Eridani's Planetary Debris Disk: Structure and Dynamics Based on Spitzer and Caltech Submillimeter Observatory Observations". The Astrophysical Journal. 690 (2): 1522–1538. arXiv:0810.4564. Bibcode:2009ApJ...690.1522B. doi:10.1088/0004-637X/690/2/1522. S2CID 18183427.
  19. ^ Brogi, M.; et al. (2009). "Dynamical stability of the inner belt around Epsilon Eridani". Astronomy and Astrophysics. 499 (2): L13–L16. Bibcode:2009A&A...499L..13B. doi:10.1051/0004-6361/200811609.
  20. ^ Reidemeister, Martin; et al. (2010). "The cold origin of the warm dust around epsilon Eridani". Astronomy & Astrophysics. 527: A57. arXiv:1011.4882. Bibcode:2011A&A...527A..57R. doi:10.1051/0004-6361/201015328. S2CID 56019152.
  21. ^ Makarov, Valeri V.; Zacharias, Norbert; Finch, Charles T. (2021). "Looking for Astrometric Signals below 20 m s−1: A Jupiter-mass Planet Signature in ε Eri". Research Notes of the AAS. 5 (6): 155. arXiv:2107.01090. Bibcode:2021RNAAS...5..155M. doi:10.3847/2515-5172/ac0f59. We conclude that the newest astrometric results confirm the existence of a long-period exoplanet orbiting ε Eri....The results are consistent with the previously reported planet epsEri-b of approximately Jupiter mass and a period of several years.
  22. ^ "Planet eps Eridani b". Extrasolar Planets Encyclopaedia. Retrieved 26 September 2021.
  23. ^ a b Llop-Sayson, Jorge; Wang, Jason J.; Ruffio, Jean-Baptiste; Mawet, Dimitri; et al. (6 October 2021). "Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multiepoch Vortex Coronagraphy Upper Limits". The Astronomical Journal. 162 (5): 181. arXiv:2108.02305. Bibcode:2021AJ....162..181L. doi:10.3847/1538-3881/ac134a. eISSN 1538-3881. ISSN 0004-6256. S2CID 236924533.
  24. ^ Rosenthal, Lee J.; Fulton, Benjamin J.; et al. (2021-07-01). "The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades". The Astrophysical Journal Supplement Series. 255 (1). American Astronomical Society: 8. arXiv:2105.11583. Bibcode:2021ApJS..255....8R. doi:10.3847/1538-4365/abe23c. ISSN 0067-0049. S2CID 235186973.
  25. ^ "First image and spectrum of a true Jupiter-Saturn Analog". STScI. Retrieved 29 February 2024. We propose to take the first image and spectrum of a true Solar System gas giant analog, the emblematic eps Eridani b, with the NIRSpec integral field unit (IFU).
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