CHEMISTRY OF SILICATE ATMOSPHERES OF EVAPORATING SUPER-EARTHS
- Planetary Chemistry Laboratory, McDonnell Center for the Space Sciences, Department of Earth and Planetary Sciences, Washington University in St. Louis, Saint Louis, MO 63130-4899 (United States)
We model the formation of silicate atmospheres on hot volatile-free super-Earths. Our calculations assume that all volatile elements such as H, C, N, S, and Cl have been lost from the planet. We find that the atmospheres are composed primarily of Na, O{sub 2}, O, and SiO gas, in order of decreasing abundance. The atmospheric composition may be altered by fractional vaporization, cloud condensation, photoionization, and reaction with any residual volatile elements remaining in the atmosphere. Cloud condensation reduces the abundance of all elements in the atmosphere except Na and K. We speculate that large Na and K clouds such as those observed around Mercury and Io may surround hot super-Earths. These clouds would occult much larger fractions of the parent star than a closely bound atmosphere, and may be observable through currently available methods.
- OSTI ID:
- 21371909
- Journal Information:
- Astrophysical Journal (Online), Vol. 703, Issue 2; Other Information: DOI: 10.1088/0004-637X/703/2/L113; ISSN 1538-4357
- Country of Publication:
- United States
- Language:
- English
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