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User:IliterateKit/Habitability of red dwarf systems

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The theorized habitability of red dwarf systems is determined by factors including tidal effects, flaring, and variability. Modern evidence suggests that planets in red dwarf systems are unlikely to be habitable, due to high probability of tidal locking, intense solar flaring activity, likely lack of atmospheres, and the high stellar variation many such planets would experience.[1] However, many recent models have proposed mechanisms through which red dwarfs can mitigate these effects. Research suggests that magnetic fields can shield planets from solar flares[2] and theoretical simulations have shown the possibility of atmospheric mechanisms that can redistribute heat from the dayside to the nightside[3]. The sheer number and longevity of red dwarfs also provides ample opportunity to research habitability.

As of 2025, arguments concerning the habitability of red dwarf systems are unresolved, and the area remains an open question of study in the fields of climate modeling and the evolution of life on Earth. Observational data and statistical arguments suggest that red dwarf systems are uninhabitable for indeterminate reasons.[4] In contrast, 3D climate models favor habitability[5] and wider habitable zones for slow rotating and tidally locked planets.

Background

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Red dwarfs[6] are the smallest, coolest, and most common type of star. Estimates of their abundance range from 70% of stars in spiral galaxies to more than 90% of all stars in elliptical galaxies,[7][8] an often quoted median figure being 72–76% of the stars in the Milky Way (known since the 1990s from radio telescopic observation to be a barred spiral).[9] Red dwarfs are usually defined as being of spectral type M, although some definitions are wider (including also some or all K-type stars). Given their low energy output, red dwarfs are almost never naked-eye visible from Earth.

This low luminosity causes the habitable zone of red dwarf systems to occur closer to the star. This helps in the detection of Earth-like exoplanets through the transit method, as the probability of an observable transit is 1.5-2.7%, much greater than the Earth-Sun system's 0.47%.[10] Detection is also not likely to be affected by stellar activity.[11]

Longevity and ubiquity

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Red dwarfs' greatest advantage as candidate stars for life is their longevity. It took 4.5 billion years for intelligent life to evolve on Earth, and life as we know it will see suitable conditions for 1[12] to 2.3[13] billion years more. Red dwarfs, by contrast, could live for hundreds of billions of years on the main sequence, as their nuclear reactions are far slower than those of larger stars.[a] Estimates suggest that 10-75% of dwarfs have Earth or super-Earth sized planets.[14] Combined with their longevity, this leaves potential for the evolution of microbial or intelligent life in the future.

Tidal effects

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The effect of tidal locking on red dwarf habitability is still debated. In order for red dwarf exoplanets to retain significant amounts of water in the habitable zone, they must orbit close to the star, and are likely tidally locked.[15] Tidal locking makes the planet rotate on its axis once every revolution around the star, meaning one side of the planet would eternally face the star and another side would perpetually face away, creating great extremes of temperature.

How fast tidal locking occurs can depend on a planet's oceans and atmosphere. This may cause tidal locking to fail to occur even after many billions of years. Further, tidal locking is not the only possible end state of tidal dampening. Mercury, for example, has had sufficient time to tidally lock, but is in a 3:2 spin orbit resonance due to an eccentric orbit.[16] Depending on the ratio, resonance can create preferentially heated regions on the planet, causing similar issues to habitability as tidal locking.[17]

For many years, it was believed that life on tidally locked planets would be limited to the terminator, where the star would always appear on or close to the horizon. It was also thought that efficient heat transfer between the sides of the planet necessitated atmospheric circulation of an atmosphere so thick as to disallow photosynthesis. Due to differential heating, a tidally locked planet would experience fierce winds with permanent torrential rain at the point directly facing the local star,[18] the sub-solar point.

Artist's impression of GJ 667 Cc, a potentially habitable planet orbiting a red dwarf constituent in a trinary star system

A 1997 study by NASA's Ames Research Center have shown that a planet's atmosphere (assuming it included greenhouse gases CO2 and H2O) need only be 100 millibar, or 10% of Earth's atmosphere, for the star's heat to be effectively carried to the night side, a figure well within the bounds of photosynthesis.[19] Subsequent research has shown that seawater could effectively circulate without freezing if the ocean basins were deep enough to allow free flow beneath the night side's ice cap. A 2010 study concluded that Earth-like water worlds tidally locked to their stars would still have temperatures above 240 K (−33 °C) on the night side.[20] Climate models constructed in 2013 indicate that cloud formation on tidally locked planets would minimize the temperature difference between the day and the night side, greatly improving habitability prospects for red dwarf planets.[21]

A 2020 model also suggested that mineral dust in the atmosphere can help mitigate the extreme temperatures on tidally locked planets. As water evaporates, less of the surface is covered in water, and the amount of mineral dust suspended in the atmosphere increases. This helps cool down the entire planet and increase the amount of water retained in the atmosphere.[22] The proposed mineral dust would obscure detection of prominent biomarker gases such as methane and ozone, and could impact assessment of red dwarf habitability.

Tidal Venuses

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Tidal heating experienced by planets in the habitable zone of red dwarfs less than 30% of the mass of the Sun may cause them to be "baked out" and become "tidal Venuses."[23] The eccentricity of over 150 planets found orbiting M dwarfs was measured, and it was found that two-thirds of these exoplanets are exposed to extreme tidal forces, rendering them uninhabitable due to the intense heat generated by tidal heating.[24]

There may be too little water for habitable planets around many red dwarfs;[25] what little water is on such planets, especially Earth-sized ones, may be located on the cold night side of the planet. In contrast to the predictions of earlier studies on tidal Venuses, this "trapped water" may help to stave off runaway greenhouse effects and improve the habitability of red dwarf systems.[26]

Variability

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Red dwarfs are far more volatile than their larger, more stable cousins. Often, they are covered in starspots that can dim their emitted light by up to 40% for months at a time. At other times, red dwarfs emit gigantic flares that can double their brightness in a matter of minutes.[27] Most red dwarfs have been classified as flare stars to some degree or other. Such variation in brightness could be very damaging for life. Recent 3D climate models simulate flare events by altering the stellar flux received by any given planet. One study found that if a tidally locked planet possess a sufficient atmosphere, cloud coverage and albedo increase monotonically with stellar flux, increasing the resilience of the planet to variations in radiation.[28] This caveat has proven difficult, however, since flares produce torrents of charged particles that could strip off sizable portions of the planet's atmosphere.[29]

Solar flaring and atmospheres

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For a planet around a red dwarf star to support life, it would require a rapidly rotating magnetic field to protect it from the flares. A tidally locked planet rotates slowly, and so may not be able to produce a geodynamo at its core. The violent flaring period of a red dwarf's life cycle is estimated to last for only about the first 1.2 billion years of its active life. If a planet forms far away from a red dwarf so as to avoid atmospheric erosion, and then migrates into the star's habitable zone after this turbulent initial period, it is possible for life to develop.[30] However, observations of the 7 to 12-billion year old Barnard's Star showcase that even old red dwarfs can have significant flare activity. Barnard's Star was long assumed to have little activity, but in 1998, astronomers observed an intense stellar flare, showing that it is a flare star.[31]

The largest flares occur at high latitudes near the stellar poles. If an exoplanet's orbit is aligned with the stellar rotation (as is the case with the planets of the Solar System), then it is less affected by the flares than formerly thought.[32]

Scientists who believe in the Rare Earth hypothesis doubt that red dwarfs could support life amid strong flaring. Tidal locking would probably result in a relatively low planetary magnetic moment, and active red dwarfs that emit coronal mass ejections (CMEs) would bow back the magnetosphere until it contacted the planetary atmosphere. As a result, the atmosphere would undergo strong erosion, possibly leaving the planet uninhabitable.[33][34][35] However, it was found that red dwarfs have a much lower CME rate than expected from their rotation or flare activity, and large CMEs are rare. This suggests that atmospheric erosion is caused mainly by radiation rather than CMEs.[36]

Otherwise, it is suggested that if the planet had a magnetic field, it would deflect the particles from the atmosphere (even the slow rotation of a tidally locked M-dwarf planet—it spins once for every time it orbits its star—would be enough to generate a magnetic field as long as part of the planet's interior remained molten).[37] This magnetic field must be much stronger than Earth's to protect against flares of the observed magnitude: 10–1000 G versus Earth's ~0.5 G. This is unlikely to be generated.[38] Mathematical models further conclude that,[39][40][41] even under the highest attainable dynamo-generated magnetic field strengths, exoplanets with masses similar to that of Earth lose a significant fraction of their atmospheres by the erosion of the exobase's atmosphere by Coronal mass ejection (CME) bursts and extreme ultraviolet (XUV) emissions (even those Earth-like planets closer than 0.8 AU, affecting also G and K stars, are prone to losing their atmospheres). Atmospheric erosion could likely trigger depletion of water oceans also.[42] Planets shrouded by a thick haze of hydrocarbons, such as the ones on primordial Earth or Saturn's moon Titan might still survive the flares, as floating droplets of hydrocarbon are particularly efficient at absorbing ultraviolet radiation.[43]

Measurements reject the presence of relevant atmospheres in two exoplanets orbiting a red dwarf: TRAPPIST-1b and TRAPPIST-1c. The two planets are bare rocks, or have very thin atmospheres.[44] The rest of the TRAPPIST-1 planets, all of whom other than the exceptions of TRAPPIST-1h or possibly TRAPPIST-1d are in the habitable zone, are unlikely to have atmospheres, but their existence is not entirely ruled out. Other potentially habitable planets orbiting red dwarfs, such as LHS 1140b[45][46] or K2-18b[47] have likely atmospheres. Calculations based in XUV fluences provide that five out of 49 planets below 1.8 Earth-radii orbiting red dwarfs within 50 parsecs would have retained an atmosphere.[48]

Another way that life could initially protect itself from radiation would be remaining underwater until the star had passed through its early flare stage, assuming the planet could retain enough of an atmosphere to sustain liquid oceans. Once life reached land, the low amount of UV produced by a quiet red dwarf means that life could thrive without an ozone layer, and thus never need to produce oxygen.[49]

Article Evaluation

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The existing article for Habitability of red dwarf systems is missing citations for large chunks of the text, and many of the citations present are on the older side. There's been a lot of contemporary research on the matter that would benefit the article. I think a list of red dwarf systems would also be useful to add so readers can easily jump off to sections for further research.

The article's tone is mostly neutral but is written a focus on the impracticality of red dwarf habitability. I'd want to update the entire section with recent sources and a more neutral viewpoint.

The talk page is rather active but most of the discussion was pre-2018. Many of the comments have to do with updating the article to line up with contemporary research. I wonder why the activity decreased so much.

Introduction

"As of 2025" is kind of just there without referencing any papers or justifying the year.

"While the likelihood of finding a planet in the habitable zone around any specific red dwarf is slight, the total amount of habitable zone around all red dwarfs combined is equal to the total amount around Sun-like stars, given their ubiquity" doesn't really make sense to me and can use significant rewording.

Tidal Effects / Variability

This entire passage is written in a winding manner and could be more efficiently written.

Methane habitable zone

I'm curious about the presence of the "Methane habitable zone" section on the page. I'd want to make it more substantive or remove it. Realistically, I'd add a section on the habitable zone for carbon based life.

Article Draft

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Lead

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Article body

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References

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  1. ↑ Childs, Anna C.; Martin, Rebecca G.; Livio, Mario (2022-10-01). "Life on Exoplanets in the Habitable Zone of M Dwarfs?". The Astrophysical Journal Letters. 937 (2): L41. doi:10.3847/2041-8213/ac9052. ISSN 2041-8205.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  2. ↑ Segura, Antígona; Walkowicz, Lucianne M.; Meadows, Victoria; Kasting, James; Hawley, Suzanne (2010-09-01). "The Effect of a Strong Stellar Flare on the Atmospheric Chemistry of an Earth-like Planet Orbiting an M Dwarf". Astrobiology. 10 (7): 751–771. doi:10.1089/ast.2009.0376. ISSN 1531-1074. PMC 3103837. PMID 20879863.
  3. ↑ Boutle, Ian A.; Joshi, Manoj; Lambert, F. Hugo; Mayne, Nathan J.; Lyster, Duncan; Manners, James; Ridgway, Robert; Kohary, Krisztian (2020-06-09). "Mineral dust increases the habitability of terrestrial planets but confounds biomarker detection". Nature Communications. 11 (1). doi:10.1038/s41467-020-16543-8. ISSN 2041-1723. PMC 7283277. PMID 32518292.
  4. ↑ Waltham, David (January 2017). "Star Masses and Star-Planet Distances for Earth-like Habitability". Astrobiology. 17 (1): 61–77. Bibcode:2017AsBio..17...61W. doi:10.1089/ast.2016.1518. PMC 5278800. PMID 28103107.
  5. ↑ Yang, Jun; Cowan, Nicolas B.; Abbot, Dorian S. (27 June 2013). "Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets". The Astrophysical Journal. 771 (2): L45. arXiv:1307.0515. Bibcode:2013ApJ...771L..45Y. doi:10.1088/2041-8205/771/2/L45. S2CID 14119086. Retrieved 30 July 2024.
  6. ↑ The term dwarf applies to all stars in the main sequence, including the Sun.
  7. ↑ van Dokkum, Pieter G.; Conroy, Charlie (1 December 2010). "A substantial population of low-mass stars in luminous elliptical galaxies". Nature. 468 (7326): 940–942. arXiv:1009.5992. Bibcode:2010Natur.468..940V. doi:10.1038/nature09578. PMID 21124316. S2CID 205222998.
  8. ↑ Yale University (December 1, 2010). "Discovery Triples Number of Stars in Universe". ScienceDaily. Archived from the original on January 4, 2019. Retrieved December 17, 2010.
  9. ↑ Dole, Stephen H. Habitable Planets for Man 1965 Rand Corporation report, published in book form--A figure of 73% is given for the percentage of red dwarfs in the Milky Way.
  10. ↑ Charbonneau, David; Deming, Drake (2007-06-07). "The Dynamics-Based Approach to Studying Terrestrial Exoplanets". arXiv.org. doi:10.48550/arXiv.0706.1047. Retrieved 2026-04-05.
  11. ↑ Shields, Aomawa L.; Ballard, Sarah; Johnson, John Asher (2016-12). "The habitability of planets orbiting M-dwarf stars". Physics Reports. 663: 1–38. doi:10.1016/j.physrep.2016.10.003. ISSN 0370-1573. {{cite journal}}: Check date values in: |date= (help)
  12. ↑ Hines, Sandra (13 January 2003). "'The end of the world' has already begun, UW scientists say" (Press release). University of Washington. Archived from the original on 11 January 2008. Retrieved 5 June 2007.
  13. ↑ Li, King-Fai; Pahlevan, Kaveh; Kirschvink, Joseph L.; Yung, Yuk L. (2009). "Atmospheric pressure as a natural climate regulator for a terrestrial planet with a biosphere" (PDF). Proceedings of the National Academy of Sciences. 106 (24): 9576–9579. Bibcode:2009PNAS..106.9576L. doi:10.1073/pnas.0809436106. PMC 2701016. PMID 19487662. Archived (PDF) from the original on 4 July 2009. Retrieved 19 July 2009.
  14. ↑ Wandel, A.; Gale, J. (2020-04). "The bio-habitable zone and atmospheric properties for planets of red dwarfs". International Journal of Astrobiology. 19 (2): 126–135. doi:10.1017/S1473550419000235. ISSN 1473-5504. {{cite journal}}: Check date values in: |date= (help)
  15. ↑ Bolmont, E.; Selsis, F.; Owen, J. E.; Ribas, I.; Raymond, S. N.; Leconte, J.; Gillon, M. (21 January 2017). "Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1". Monthly Notices of the Royal Astronomical Society. 464 (3): 3728–3741. arXiv:1605.00616. Bibcode:2017MNRAS.464.3728B. doi:10.1093/mnras/stw2578.
  16. ↑ Kasting, James F.; Whitmire, Daniel P.; Reynolds, Ray T. (1993). "Habitable Zones around Main Sequence Stars" (PDF). Icarus. 101 (1): 108–128. Bibcode:1993Icar..101..108K. doi:10.1006/icar.1993.1010. PMID 11536936. Archived (PDF) from the original on 2023-04-26. Retrieved 2017-08-03.
  17. ↑ Colose, Christopher M.; Haqq-Misra, Jacob; Wolf, Eric T.; Del Genio, Anthony D.; Barnes, Rory; Way, Michael J.; Ruedy, Reto (2021-11-01). "Effects of Spin–Orbit Resonances and Tidal Heating on the Inner Edge of the Habitable Zone". The Astrophysical Journal. 921 (1): 25. doi:10.3847/1538-4357/ac135c. ISSN 0004-637X.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  18. ↑ Joshi, M. (2003). "Climate model studies of synchronously rotating planets". Astrobiology. 3 (2): 415–427. Bibcode:2003AsBio...3..415J. doi:10.1089/153110703769016488. PMID 14577888.
  19. ↑ Joshi, M. M.; Haberle, R. M.; Reynolds, R. T. (October 1997). "Simulations of the Atmospheres of Synchronously Rotating Terrestrial Planets Orbiting M Dwarfs: Conditions for Atmospheric Collapse and the Implications for Habitability" (PDF). Icarus. 129 (2): 450–465. Bibcode:1997Icar..129..450J. doi:10.1006/icar.1997.5793. Archived from the original (PDF) on 2014-07-15. Retrieved 2007-08-11.
  20. ↑ Merlis, T. M.; Schneider, T. (2010). "Atmospheric dynamics of Earth-like tidally locked aquaplanets". Journal of Advances in Modeling Earth Systems. 2 (4) JAMES.2010.2.13: n/a. arXiv:1001.5117. Bibcode:2010JAMES...2...13M. doi:10.3894/JAMES.2010.2.13. S2CID 37824988.
  21. ↑ Yang, Jun; Cowan, Nicolas B.; Abbot, Dorian S. (27 June 2013). "Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets". The Astrophysical Journal. 771 (2): L45. arXiv:1307.0515. Bibcode:2013ApJ...771L..45Y. doi:10.1088/2041-8205/771/2/L45. S2CID 14119086. Retrieved 30 July 2024.
  22. ↑ Boutle, Ian A.; Joshi, Manoj; Lambert, F. Hugo; Mayne, Nathan J.; Lyster, Duncan; Manners, James; Ridgway, Robert; Kohary, Krisztian (2020-06-09). "Mineral dust increases the habitability of terrestrial planets but confounds biomarker detection". Nature Communications. 11 (1): 2731. doi:10.1038/s41467-020-16543-8. ISSN 2041-1723. PMC 7283277. PMID 32518292.
  23. ↑ Barnes, Rory; Mullins, Kristina; Goldblatt, Colin; Meadows, Victoria S.; Kasting, James F.; Heller, René (March 2013). "Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating". Astrobiology. 13 (3): 225–250. arXiv:1203.5104. Bibcode:2013AsBio..13..225B. doi:10.1089/ast.2012.0851. PMC 3612283. PMID 23537135.
  24. ↑ Sagear, Sheila; Ballards, Sarah (2023). "The Orbital Eccentricity Distribution of Planets Orbiting M dwarfs". PNAS. XXX (XX) e2217398120. arXiv:2305.17157. Bibcode:2023PNAS..12017398S. doi:10.1073/pnas.2217398120. PMC 10265968. PMID 37252955. S2CID 258960478.
  25. ↑ Lissauer, Jack J. (2007). "Planets formed in habitable zones of M dwarf stars probably are deficient in volatiles". The Astrophysical Journal. 660 (2): 149–152. arXiv:astro-ph/0703576. Bibcode:2007ApJ...660L.149L. doi:10.1086/518121. S2CID 12312927.
  26. ↑ Menou, Kristen (16 August 2013). "Water-Trapped Worlds". The Astrophysical Journal. 774 (1): 51. arXiv:1304.6472. Bibcode:2013ApJ...774...51M. doi:10.1088/0004-637X/774/1/51. S2CID 118363386.
  27. ↑ Croswell, Ken (27 January 2001). "Red, willing and able". New Scientist. Archived from the original on 2008-04-30. Retrieved 2007-08-05.
  28. ↑ Yang, Jun; Cowan, Nicolas B.; Abbot, Dorian S. (27 June 2013). "Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets". The Astrophysical Journal. 771 (2): L45. arXiv:1307.0515. Bibcode:2013ApJ...771L..45Y. doi:10.1088/2041-8205/771/2/L45. S2CID 14119086. Retrieved 30 July 2024.
  29. ↑ Guinan, Edward F.; Engle, S. G.: "Future Interstellar Travel Destinations: Assessing the Suitability of Nearby Red Dwarf Stars as Hosts to Habitable Life-bearing Planets"; American Astronomical Society, AAS Meeting #221, #333.02 Publication Date:01/2013 Bibcode:2013AAS...22133302G
  30. ↑ Cain, Fraser; Gay, Pamela (2007). "AstronomyCast episode 40: American Astronomical Society Meeting, May 2007". Universe Today. Archived from the original on 2012-03-12. Retrieved 2018-09-06.
  31. ↑ Croswell, Ken (November 2005). "A Flare for Barnard's Star". Astronomy Magazine. Kalmbach Publishing Co. Archived from the original on 2015-02-24. Retrieved 2006-08-10.
  32. ↑ Ilin, Ekaterina; Poppenhaeger, Katja; et al. (5 August 2021). "Giant white-light flares on fully convective stars occur at high latitudes". Monthly Notices of the Royal Astronomical Society. 507 (2): 1723–1745. arXiv:2108.01917. doi:10.1093/mnras/stab2159.
  33. ↑ Khodachenko, Maxim L.; et al. (2007). "Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. I. CME Impact on Expected Magnetospheres of Earth-Like Exoplanets in Close-In Habitable Zones". Astrobiology. 7 (1): 167–184. Bibcode:2007AsBio...7..167K. doi:10.1089/ast.2006.0127. PMID 17407406.
  34. ↑ Kay, C.; et al. (2016). "Probability of Cme Impact on Exoplanets Orbiting M Dwarfs and Solar-Like Stars". The Astrophysical Journal. 826 (2): 195. arXiv:1605.02683. Bibcode:2016ApJ...826..195K. doi:10.3847/0004-637X/826/2/195. S2CID 118669187.
  35. ↑ Garcia-Sage, K.; et al. (2017). "On the Magnetic Protection of the Atmosphere of Proxima Centauri b". The Astrophysical Journal Letters. 844 (1): L13. Bibcode:2017ApJ...844L..13G. doi:10.3847/2041-8213/aa7eca. S2CID 126391408.
  36. ↑ K., Vida (2019). "The quest for stellar coronal mass ejections in late-type stars. I. Investigating Balmer-line asymmetries of single stars in Virtual Observatory data". Astronomy & Astrophysics. 623 (14): A49. arXiv:1901.04229. Bibcode:2019A&A...623A..49V. doi:10.1051/0004-6361/201834264. S2CID 119095055.
  37. ↑ Alpert, Mark (November 1, 2005). "Red Star Rising: Small, cool stars may be hot spots for life". Scientific American. 293 (5): 28. Bibcode:2005SciAm.293e..28A. doi:10.1038/scientificamerican1105-28. PMID 16318021. Archived from the original on 2022-02-12. Retrieved 2013-01-19.
  38. ↑ K., Vida (2017). "Frequent flaring in the TRAPPIST-1 system - unsuited for life?". The Astrophysical Journal. 841 (2): 124. arXiv:1703.10130. Bibcode:2017ApJ...841..124V. doi:10.3847/1538-4357/aa6f05. S2CID 118827117.
  39. ↑ Zuluaga, J. I.; Cuartas, P. A.; Hoyos, J. H. (2012). "Evolution of magnetic protection in potentially habitable terrestrial planets". arXiv:1204.0275 [astro-ph.EP].
  40. ↑ See, V.; Jardine, M.; Vidotto, A. A.; Petit, P.; Marsden, S. C.; Jeffers, S. V.; do Nascimento, J. D. (30 October 2014). "The effects of stellar winds on the magnetospheres and potential habitability of exoplanets". Astronomy & Astrophysics. 570: A99. arXiv:1409.1237. Bibcode:2014A&A...570A..99S. doi:10.1051/0004-6361/201424323. S2CID 16146794.
  41. ↑ Dong, Chuanfei; Lingam, Manasvi; Ma, Yingjuan; Cohen, Ofer (10 March 2017). "Is Proxima Centauri b Habitable? A Study of Atmospheric Loss". The Astrophysical Journal Letters. 837:L26 (2): L26. arXiv:1702.04089. Bibcode:2017ApJ...837L..26D. doi:10.3847/2041-8213/aa6438. S2CID 118927765.
  42. ↑ Dong, Chuanfei; et al. (2017). "The dehydration of water worlds via atmospheric losses". The Astrophysical Journal Letters. 847 (L4): L4. arXiv:1709.01219. Bibcode:2017ApJ...847L...4D. doi:10.3847/2041-8213/aa8a60. S2CID 119424858.
  43. ↑ Tilley, Matt A; et al. (22 Nov 2017). "Modeling Repeated M-dwarf Flaring at an Earth-like Planet in the Habitable Zone: I. Atmospheric Effects for an Unmagnetized Planet". Astrobiology. 19 (1): 64–86. arXiv:1711.08484. doi:10.1089/ast.2017.1794. PMC 6340793. PMID 30070900.
  44. ↑ Zleba, Sebastian; Kreldberg, Laura (19 June 2023). "No thick carbon dioxide atmosphere on the rocky exoplanet TRAPPIST-1 c". Nature. 620 (7975): 746–749. arXiv:2306.10150. Bibcode:2023Natur.620..746Z. doi:10.1038/s41586-023-06232-z. PMC 10447244. PMID 37337068. S2CID 259200424.
  45. ↑ Damiano, Mario; Bello-Arufe, Aaron; et al. (March 2024). "LHS 1140 b is a Potentially Habitable Water World". The Astrophysical Journal Letters. 968 (2): L22. arXiv:2403.13265. Bibcode:2024ApJ...968L..22D. doi:10.3847/2041-8213/ad5204.
  46. ↑ "Habitable Zone Exoplanet LHS 1140b is Probably Snowball or Water World | Sci.News". Sci.News: Breaking Science News. 2024-07-09. Retrieved 2024-07-10.
  47. ↑ Madhusudhan, Nikku; Nixon, Matthew C.; Welbanks, Luis; Piette, Anjali A. A.; Booth, Richard A. (February 2020). "The Interior and Atmosphere of the Habitable-zone Exoplanet K2-18b". The Astrophysical Journal Letters. 891 (1): L7. arXiv:2002.11115. Bibcode:2020ApJ...891L...7M. doi:10.3847/2041-8213/ab7229. ISSN 2041-8205. S2CID 211505592.
  48. ↑ Emily K Pass; Charbonneau, David; Vanderburg, Andrew (2025). "The Receding Cosmic Shoreline of Mid-to-Late M Dwarfs: Measurements of Active Lifetimes Worsen Challenges for Atmosphere Retention by Rocky Exoplanets". The Astrophysical Journal. 986 (1): L3. arXiv:2504.01182. Bibcode:2025ApJ...986L...3P. doi:10.3847/2041-8213/adda39.
  49. ↑ Kiang, Nancy Y. (April 2008). "The color of plants on other worlds". Scientific American. 298 (4): 48–55. Bibcode:2008SciAm.298d..48K. doi:10.1038/scientificamerican0408-48. PMID 18380141. S2CID 12329051.
  1. ↑ The more massive a star is, the shorter it lives.
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