40 Eridani is a triple star system in the constellation of Eridanus, abbreviated 40 Eri. It has the Bayer designation Omicron2 Eridani, which is Latinized from ο2 Eridani and abbreviated Omicron2 Eri or ο2 Eri. Based on parallax measurements taken by the Gaia mission, it is about 16.3 light-years (5.0 parsecs) from the Sun.

The primary star of the system, designated 40 Eridani A and formally named Keid,[1] is easily visible to the naked eye, with an apparent magnitude of 4.43.[2] It is orbited by a binary pair whose two components are designated 40 Eridani B and C, and which were discovered on January 31, 1783, by William Herschel.[3]: p73 It was again observed by Friedrich Struve in 1825 and by Otto Struve in 1851.[4][5]

In 1910, it was discovered that although 40 Eridani B was a faint star, it was white in color. This meant that it had to be a small star; in fact it was a white dwarf, the first discovered.[6] Although it is neither the closest white dwarf, nor the brightest in the night sky, it is by far the easiest to observe; it is nearly three magnitudes brighter than Van Maanen's Star, the nearest solitary white dwarf, and unlike the companions of Procyon and Sirius it is not outshone by the glare of a much brighter primary.[7]

Nomenclature

40 Eridani is the system's Flamsteed designation and ο2 Eridani (Latinised to Omicron2 Eridani) its Bayer designation. The designations of the sub-components – 40 Eridani A, B and C – derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[8] 40 Eridani C also bears the variable star designation DY Eridani.

The system bore the traditional name Keid derived from the Arabic word القيض (alqayḍ) meaning "the eggshells", alluding to its neighbour Beid (Arabic "egg").[9] In 2016, the IAU organized a Working Group on Star Names (WGSN)[10] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[11] It approved the name Keid for the component 40 Eridani A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.[1]

Properties

40 Eridani A is a main-sequence dwarf of spectral type K0.5, 40 Eridani B is a 9th magnitude white dwarf of spectral type DA4, and 40 Eridani C is an 11th magnitude red dwarf flare star of spectral type M4.5e. When component B was a main-sequence star, it is thought to have been the most massive member of the system at 1.8 solar mass, but ejected much of its mass before it became a white dwarf.[12] B and C orbit each other approximately 400 AU from the primary star, A.[13] Their orbit has a semimajor axis of 35 AU and is rather elliptical with an orbital eccentricity of 0.410.[4]

Potential for life

The habitable zone of 40 Eridani A, where a planet could exist with liquid water, is near 0.68 AU from A. At this distance a planet would complete a revolution in 223 Earth days (according to the third of Kepler's laws) and 40 Eridani A would appear nearly 20%[note 1] wider than the Sun does on Earth. An observer on a planet in the 40 Eridani A system would see the B–C pair as unusually bright white and reddish-orange stars in the night sky – magnitudes −8 and −6, slightly brighter than the appearance of Venus seen from Earth as the evening star.

It is unlikely that habitable planets exist around 40 Eridani B because they would have been sterilized by its evolution into a white dwarf. As for 40 Eridani C, it is prone to flares, which cause large momentary increases in the emission of X-rays as well as visible light. This would be lethal to Earth-type life on planets near the flare star.[13]

Search for planets

40 Eridani A shows periodic radial velocity variations, which were suggested to be caused by a planetary companion. The 42-day period is close to the stellar rotation period, which made the possible planetary nature of the signal difficult to confirm.[14] A 2018 study found that most evidence supports a planetary origin for the signal,[15] but this was controversial, with a 2021 study characterizing the signal as a false positive,[16] and a 2022 study getting inconclusive results.[17] Further studies in 2023[18]: 23–24,44 and 2024 concluded that the radial velocity signal very likely does originate from stellar activity, and not from a planet.[19]

The candidate planet would have had a minimum mass of 8.47 ± 0.47 Earth mass, and lie considerably interior to the habitable zone, receiving nine times more stellar flux than Earth, which is an even greater amount than Mercury, the innermost planet in the Solar System, on average receives from the Sun.[15]

Appearance of the Solar System

As seen from the 40 Eridani system, the Sun is a 3.4-magnitude star in Hercules, near the border with Serpens Caput.[note 2]

In fiction

In the Star Trek franchise, the planet Vulcan orbits 40 Eridani A.[20] Vulcan has been referenced in relation to the real-life search for exoplanets in this system.[21][19]

The hypothetical planet 40 Eridani A b is also mentioned in the book Project Hail Mary as the home of the eponymous Eridian species.[22] The planet is called "Erid" in both the book and its 2026 film adaptation.[23]

In the Dune franchise the fourth planet of 40 Eridani A is an inhabited[24] and technologically advanced planet called Richese.

In the Bobiverse series by Dennis E. Taylor, a double planet is found orbiting 40 Eridani A,[25] and named Vulcan and Romulus by an uploaded intelligence in a von Neumann probe.

Notes

  1. ^ From \ h = \frac{\ a\ }{d} \,, where h is the apparent height, d is the distance of the object, and a is the actual size of the object.
  2. ^ From 40 Eridani the Sun would appear on the diametrically opposite side of the sky at the coordinates RA=, Dec=, which is located near the border of Hercules (constellation) and Serpens Caput, the closest bright star being Alpha Serpentis. The absolute magnitude of the Sun is 4.85, so, at a distance of 5.04 parsecs, the Sun would have an apparent magnitude \begin{smallmatrix}m\ =\ M_v\ +\ 5\cdot((\log_{10}\ 5.04)\ -\ 1)\ =\ 3.36\end{smallmatrix}.

See also

References

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  2. ^ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600
  3. ^ Herschel, William (1785). "Catalogue of Double Stars. By William Herschel, Esq. F. R. S". Philosophical Transactions of the Royal Society of London. 75: 40–126. Bibcode:1785RSPT...75...40H. doi:10.1098/rstl.1785.0006. JSTOR 106749. S2CID 186209747
  4. ^ Heintz, W. D. (1974). "Astrometric study of four visual binaries". Astronomical Journal. 79: 819. Bibcode:1974AJ.....79..819H. doi:10.1086/111614
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  8. ^ Hessman, F.V.; Dhillon, V.S.; Winget, D.E.; Schreiber, M.R.; Horne, K.; Marsh, T.R. et al. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707
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  11. ^ Working Group on Star Names Triennial Report (2015-2018). International Astronomical Union. 2018. p. 5. Archived from the original on 2022-10-09. Retrieved 2018-07-14.
  12. ^ Bond, Howard E.; Bergeron, P.; Bédard, A. (October 2017). "Astrophysical Implications of a New Dynamical Mass for the Nearby White Dwarf 40 Eridani B". The Astrophysical Journal. 848 (1): 16. arXiv:1709.00478. Bibcode:2017ApJ...848...16B. doi:10.3847/1538-4357/aa8a63. S2CID 119257982. 16.
  13. ^ "40 Eridani 3 (Omicron² Eridani)". solstation.com. Archived from the original on 30 September 2023. Retrieved 2018-02-06.
  14. ^ Díaz, Matías R.; Jenkins, James S.; Tuomi, Mikko; Butler, R. Paul; Soto, Maritza G.; Teske, Johanna K.; Feng, Fabo; Shectman, Stephen A.; Arriagada, Pamela; Crane, Jeffrey D.; Thompson, Ian B.; Vogt, Steven S. (2018). "The test case of HD26965: Difficulties disentangling weak Doppler signals from stellar activity". The Astronomical Journal. 155 (3): 126. arXiv:1801.03970. Bibcode:2018AJ....155..126D. doi:10.3847/1538-3881/aaa896. S2CID 119404519
  15. ^ Ma, Bo et al. (2018). "The first super-Earth Detection from the High Cadence and High Radial Velocity Precision Dharma Planet Survey". Monthly Notices of the Royal Astronomical Society. 480 (2): 2411. arXiv:1807.07098. Bibcode:2018MNRAS.480.2411M. doi:10.1093/mnras/sty1933
  16. ^ Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (2021). "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): 8. arXiv:2105.11583. Bibcode:2021ApJS..255....8R. doi:10.3847/1538-4365/abe23c. S2CID 235186973
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