What makes a planet habitable?

By H. Lammer, J. Bredehöft, A. Coustenis, M. Khodachenko, L. Kaltenegger, O. Grasset, D. Prieur, F. Raulin, Pascale Ehrenfreund, M. Yamauchi and 7 more. 2009

344 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/1b13fe12467753d5e14cab35cec949f28fefce5e

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Citations in the corpus

Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “From this review, one can see that there were at least 3 major periods in Earth’s evolution, which have been essential for the development of a class I habitat, as described in Lammer et al. (2009).”
ABIOTIC OXYGEN-DOMINATED ATMOSPHERES ON TERRESTRIAL HABITABLE ZONE PLANETS (2014, background): “Delivery and removal of volatiles on terrestrial planets is dependent on an array of complex, chaotic processes, so wide variations in inventories should be expected (Raymond et al. 2006; Lichtenegger et al. 2010; Lammer et al. 2009).”
WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES (2013, unknown): “However, even this mechanism could become problematic if the ocean volume is so large that pressures at the seaﬂoor are high enough to inhibit outgassing (e.g., Lammer et al. 2009).”
The Surface UV Environment on Planets Orbiting M Dwarfs: Implications for Prebiotic Chemistry and the Need for Experimental Follow-up (2017, background): “Most habitability studies of Mdwarfs treat UV radiation as a negative for habitability (Heath et al. 1999; Tarter et al. 2007; Lammer et al. 2009; Meadows et al. 2016; Shields et al. 2016), motivated by the observation that UV radiation has deleterious effects on modern life (Setlow 1974).”
Origin and loss of nebula-captured hydrogen envelopes from ‘sub’- to ‘super-Earths’ in the habitable zone of Sun-like stars (2014, methodology): “Namely, we use a lower value for η of 15% (Chassefière 1996a; 1996b; Yelle 2004; Lammer et al. 2009a; Leitzinger et al. 2011; Erkaev et al. 2013a) and a higher η value of 40% (Yelle 2004; Penz et al. 2008; Erkaev et al. 2013a; Koskinen et al. 2013; Lammer et al. 2013a).”
Is Proxima Centauri b Habitable? A Study of Atmospheric Loss (2017, background): “The Habitable Zone (HZ) is broadly defined as the region around a star where a planet can support liquid water for certain values of the atmospheric pressure (Lammer et al. 2009), and has been extensively investigated (e.g. Kasting et al. 1993; Kasting & Catling 2003; Kopparapu et al. 2013).”
The habitability of Proxima Centauri b II. Possible climates and Observability (2016, background): “Above such water inventories, Proxima b could thus be at least considered a class III or IV (if there is enough water to form high pressure ices) habitable planet (Lammer et al. 2009; Forget 2013).”
The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “While planets orbiting older M-dwarf stars may receive similar XUV emission levels to that received by the Earth (Guinan et al., 2016), M-dwarf stars exhibit saturated emission levels for the first 0.5–1 Gyr, or longer for later-type M stars (Lammer et al., 2009).”
The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present (2016, background): “Numerous studies (e.g., Lammer et al. 2009) have highlighted the impact of the so-called XUV flux on the volatile inventory of a planet, including water.”