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Molecules, Dust and Ices in Brown Dwarf Atmospheres

Published online by Cambridge University Press:  18 July 2017

S. K. Leggett ,
P. Tremblin ,
D. Saumon ,
M. S. Marley ,
C. V. Morley ,
D. S. Amundsen ,
I. Baraffe  and
G. Chabrier
S. K. Leggett
Affiliation:
Gemini Observatory, HIUSA
P. Tremblin
Affiliation:
Univ. of Exeter, UK
D. Saumon
Affiliation:
Los Alamos National Laboratory, NMUSA
M. S. Marley
Affiliation:
NASA Ames Research Center, CA USA
C. V. Morley
Affiliation:
UC Santa Cruz, CA USA
D. S. Amundsen
Affiliation:
Univ. of Exeter, UK
I. Baraffe
Affiliation:
Univ. of Exeter, UK Ens-Lyon, France
G. Chabrier
Affiliation:
Univ. of Exeter, UK Ens-Lyon, France
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Jupiter-sized brown dwarfs are found in the solar neighborhood with effective temperature Teff as low as 250 K [1]. Iron, silicates, chlorides and sulfides condense in the atmospheres of the Teff ≈ 2000 K L-type and Teff ≈ 1000 K T-type dwarfs [2]. At the T-/Y-type boundary, Teff ≈ 500 K and atmospheres are clear [3]. The next species to condense are H2O at Teff ≈ 350 K and NH3 at Teff ≈ 200 K [4].

Type
Addendum
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29A: Astronomy in Focus , August 2015 , E22
Copyright
Copyright © International Astronomical Union 2017 

References

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