Astronomy:K2-332 b

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Short description: Potentially habitable exoplanet
K2-332 b
Discovery
Discovery date2016
Orbital characteristics
Eccentricity<0.05
Orbital period17.7 days
Physical characteristics
Mean radius2.2 R🜨
Mass5.47 M🜨
Mean density2.83 g/cm3
Physics266 K


K2-332 b (also EPIC 211579112.01)[1][2] is a potentially habitable Super-Earth or Mini-Neptune exoplanet with a radius of 2.2 earths. It is in the empirical habitable zone, receiving 1.17 times the light that Earth gets from the sun. Its star, K2-332, is type M4V, with a temperature of ~3300 K.[3] It was detected using the transit method in 2016 and is 402 light-years away.[4]

Discovery

The planet is confirmed to exist and was discovered by the K2 "Second Light" mission in 2016. It was originally referred to by its EPIC designation. The average transit time is 2 hours and 2 minutes and the average depth is 0.6508%.[1][2][4][5] The object's star is within the 2MASS catalog.[5]

Characteristics

Mass, radius, and temperature

The planet has an estimated mass of 5.47 earths, and at a radius of more than twice that of the Earth, the density corresponds to that of a watery or gaseous Mini-Neptune rather than a rocky Super-Earth. It has an equilibrium temperature of 266 K (−7 °C; 19 °F), somewhat higher than Earth's.[3][5]

Orbit and host star

The planet orbits within the inner part of the habitable zone, about 1/3 of the way between the runaway G limit for Super-Earths and the absolute inner edge. Its orbital period is 17.7 days, but the planet has an unknown semi-major axis. Its star is a dim red dwarf with about 20% the mass and size of the sun. In its habitable-zone orbit, the planet receives 1.17 times the insolation Earth gets from the sun.[1][2][3][4][5]

Habitability

General habitability and atmosphere

The planet is large (over 2 Earth-radii) and has a low density consistent with that of a watery or Neptune-like planet and not a silicate planet or a partially metallic planet like Earth. This compromises its habitability, for a solid surface is required for life to develop spontaneously on a planet.[3][4][5]

However, 2021 studies show that sub-Neptunes have an abundance of water and life-friendly molecules (nitrogen, oxygen, CO2, etc.) in their atmospheres, and the area with habitable temperatures and pressures is fairly stable. As a result, K2-332 b could be a habitable planet despite its extremely low density. If the system has a leftover dust disk or asteroid/comet belt, panspermia of microbial life from a terrestrial planet or earthlike moon could occur, and the organisms would have enough time to reproduce before dying due to the harsh conditions.[6] 2019 studies of the TOI-270 system support the notion that Mini-Neptunes have life-friendly atmospheres rich in organic matter.[7]

Tidal locking

The planet is very close to its star with a low eccentricity, so it is likely to be tidally locked, with one side always facing the star. In this case, the dayside would be extremely hot, while the nightside would be cold enough to freeze an atmosphere on a terrestrial planet, where the terminator line and adjacent twilight region would be the only habitable parts of the planet. This occurs in 4.5 Gyrs in planets orbiting stars M1 and later, and in 1 Gyr in planets around stars M7 and later.[8] However, oceanic currents and wind can distribute heat evenly around a planet (any planet, not just an Earth-size one), warming the nightside past the freezing point of the atmosphere and cooling the dayside to below 100 °C. The area in the life-friendly pressure tier of the atmosphere that would also have habitable temperatures would then extend to 55° in both hemispheres on the dayside and around the nightside near the equator, with a maximum temperature of ~42 °F (6 °C). For higher levels of carbon dioxide, this area could even extend around the entire planet (minus the nadir and high polar regions).[9]

See also

References

  1. ↑ 1.0 1.1 1.2 "37 new validated planets in overlapping K2 campaigns". https://academic.oup.com/mnras/article/508/1/195/6352342. 
  2. ↑ 2.0 2.1 2.2 "Transiting exoplanet candidates from K2 Campaigns 5 and 6". https://academic.oup.com/mnras/article/461/4/3399/2608551. 
  3. ↑ 3.0 3.1 3.2 3.3 "PHL @ UPR Arecibo - The Habitable Exoplanets Catalog" (in en-US). https://phl.upr.edu/projects/habitable-exoplanets-catalog. 
  4. ↑ 4.0 4.1 4.2 4.3 "Exoplanet-catalog" (in en). https://exoplanets.nasa.gov/exoplanet-catalog/7972/k2-332-b/. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 "K2-332 | NASA Exoplanet Archive". https://exoplanetarchive.ipac.caltech.edu/overview/K2-332%20b#planet_K2-332-b_collapsible. 
  6. ↑ Koberlein, Brian; Today, Universe. "Could life exist in the atmosphere of a sub-Neptune planet?" (in en). https://phys.org/news/2021-06-life-atmosphere-sub-neptune-planet.html. 
  7. ↑ "Properties of sub-Neptune atmospheres: TOI-270 system". https://academic.oup.com/mnras/article/495/1/962/5828086. 
  8. ↑ Barnes, Rory (2017-12-01). "Tidal locking of habitable exoplanets" (in en). Celestial Mechanics and Dynamical Astronomy 129 (4): 509–536. doi:10.1007/s10569-017-9783-7. ISSN 1572-9478. Bibcode: 2017CeMDA.129..509B. https://doi.org/10.1007/s10569-017-9783-7. 
  9. ↑ Hu, Yongyun; Yang, Jun (2014-01-14). "Role of ocean heat transport in climates of tidally locked exoplanets around M dwarf stars" (in en). Proceedings of the National Academy of Sciences 111 (2): 629–634. doi:10.1073/pnas.1315215111. ISSN 0027-8424. PMID 24379386. Bibcode: 2014PNAS..111..629H. 



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