Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars III. Iron, Magnesium, and Silicon - Astrophysics > Earth and Planetary AstrophysicsReportar como inadecuado




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Abstract: We use thermochemical equilibrium calculations to model iron, magnesium, andsilicon chemistry in the atmospheres of giant planets, brown dwarfs, extrasolargiant planets EGPs, and low-mass stars. The behavior of individual Fe-, Mg-,and Si-bearing gases and condensates is determined as a function oftemperature, pressure, and metallicity. Our results are thus independent of anyparticular model atmosphere. The condensation of Fe metal strongly affects ironchemistry by efficiently removing Fe-bearing species from the gas phase.Monatomic Fe is the most abundant Fe-bearing gas throughout the atmospheres ofEGPs and L dwarfs and in the deep atmospheres of giant planets and T dwarfs.Mg- and Si-bearing gases are effectively removed from the atmosphere byforsterite Mg2SiO4 and enstatite MgSiO3 cloud formation. Monatomic Mg isthe dominant magnesium gas throughout the atmospheres of EGPs and L dwarfs andin the deep atmospheres of giant planets and T dwarfs. Silicon monoxide SiOis the most abundant Si-bearing gas in the deep atmospheres of brown dwarfs andEGPs, whereas SiH4 is dominant in the deep atmosphere of Jupiter and other gasgiant planets. Several other Fe-, Mg-, and Si-bearing gases become increasinglyimportant with decreasing effective temperature. In principle, a number of Fe,Mg, and Si gases are potential tracers of weather or diagnostic of temperaturein substellar atmospheres.



Autor: Channon Visscher, Katharina Lodders, Bruce Fegley Jr

Fuente: https://arxiv.org/



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