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Proxima Centauri d

Coordinates: Sky map 14h 29m 42.9487s, −62° 40′ 46.141″
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Proxima Centauri d
Artistic depiction of Proxima Centauri d, with Proxima Centauri and Alpha Centauri A & B visible in the background
Discovery[1]
Discovery siteVLT-ESPRESSO
Discovery date2020
Radial velocity
Orbital characteristics[1]
0.02885+0.00019
−0.00022 AU
Eccentricity0.04+0.15
−0.04
5.122+0.002
−0.0036 d
Semi-amplitude0.39±0.07 m/s
StarProxima Centauri
Physical characteristics[1]
~0.81±0.08 R🜨
Mass≥0.26±0.05 M🜨
Temperature360 K (87 °C; 188 °F)

Proxima Centauri d (also called Proxima d) is a candidate[2][1] exoplanet orbiting the red dwarf star Proxima Centauri, the closest star to the Sun and part of the Alpha Centauri triple star system. Together with two other planets[a] in the Proxima Centauri system, it is the closest known exoplanet to the Solar System, located approximately 4.2 light-years (1.3 parsecs; 40 trillion kilometres; 25 trillion miles) away in the constellation of Centaurus. The first signs of the exoplanet emerged as a weak 5.15-day signal in radial velocity data taken from the Very Large Telescope during a 2020 study on Proxima b's mass. This signal was formally proposed to be a candidate exoplanet by Faria et al. in a follow-up paper published in February 2022.[4][1]

Proxima d is a sub-Earth at least one-quarter of the mass of Earth (or twice the mass of Mars), orbiting at roughly 0.029 AU (4.3 million km; 2.7 million mi) every 5.1 days.[4] It is the least massive and innermost known planet of the Proxima Centauri system. It is the least massive exoplanet detected with the radial velocity method as of 2022. Its proximity to the star and short orbital period of 5.1 days suggest that it is likely tidally locked due to strong tidal forces. Although Proxima d orbits too close to its star to have a habitable equilibrium temperature (which likely reaches 360 K (87 °C; 188 °F)[1] from about 190% of Earth's irradiation—assuming an Earth-like reflectivity, it is theoretically possible that Proxima d possesses polar regions with habitable temperatures.

Proxima d is considered a candidate exoplanet by its discoverers and the NASA Exoplanet Archive, because it has not been independently confirmed by more than one observatory.[1][2] On the other hand, some astronomers regard Proxima d as confirmed because it could be detected via different methods of measuring the same radial velocity data from which Proxima d was discovered.[5] As of 2022, Proxima d has been detected by the ESPRESSO spectrograph on the Very Large Telescope,[1]: 9  and also at a 2σ level (which does not constitute confirmation) by the HARPS spectrograph at the La Silla Observatory.[5]

See also

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Notes

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  1. ^ Proxima Centauri c's radial velocity signature was disputed in a 2022 study, which instead attributed its detection to potential bias in data processing methods, thereby leaving its existence as disputed.[3]

References

[edit]
  1. ^ a b c d e f g h Faria, J. P.; Suárez Mascareño, A.; et al. (4 January 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. European Southern Observatory: 17. arXiv:2202.05188. Bibcode:2022A&A...658A.115F. doi:10.1051/0004-6361/202142337.
  2. ^ a b "alf Cen Overview". NASA Exoplanet Archive. NASA. Retrieved 24 September 2024.
  3. ^ Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; et al. (23 June 2022). "Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry". The Astronomical Journal. 164:84 (3) (published 8 August 2022): 18pp. arXiv:2207.13524. Bibcode:2022AJ....164...84A. doi:10.3847/1538-3881/ac7ce6.
  4. ^ a b Suárez Mascareño, A.; Faria, J. P.; et al. (11 May 2020). "Revisiting Proxima with ESPRESSO". Astronomy & Astrophysics. 639: 24. arXiv:2005.12114. Bibcode:2020A&A...639A..77S. doi:10.1051/0004-6361/202037745. ISSN 0004-6361.
  5. ^ a b Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; Donati, Jean-François; et al. (September 2022). "Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry". The Astronomical Journal. 164: 18. arXiv:2207.13524. Bibcode:2022AJ....164...84A. doi:10.3847/1538-3881/ac7ce6. 84.


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