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Author Line, Michael R. ♦ Marley, Mark S. ♦ Freedman, Richard ♦ Liu, Michael C. ♦ Burningham, Ben ♦ Morley, Caroline V. ♦ Hinkel, Natalie R. ♦ Teske, Johanna ♦ Fortney, Jonathan J. ♦ Lupu, Roxana
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ ABUNDANCE ♦ ALKALI METALS ♦ AMMONIA ♦ ATMOSPHERES ♦ CARBON ♦ CARBON DIOXIDE ♦ CARBON MONOXIDE ♦ DWARF STARS ♦ EQUILIBRIUM ♦ GRAVITATION ♦ HYDROGEN SULFIDES ♦ METHANE ♦ OXYGEN ♦ RADIANT HEAT TRANSFER ♦ SPECTRA ♦ STARS ♦ SURFACES ♦ WATER
Abstract Brown dwarf spectra are rich in information revealing of the chemical and physical processes operating in their atmospheres. We apply a recently developed atmospheric retrieval tool to an ensemble of late-T dwarf (600–800 K) near-infrared (1–2.5 μ m) spectra. With these spectra we are able to directly constrain the molecular abundances for the first time of H{sub 2}O, CH{sub 4}, CO, CO{sub 2}, NH{sub 3}, H{sub 2}S, and Na+K, surface gravity, effective temperature, thermal structure, photometric radius, and cloud optical depths. We find that ammonia, water, methane, and the alkali metals are present and that their abundances are well constrained in all 11 objects. We find no significant trend in the water, methane, or ammonia abundances with temperature, but find a very strong (>25 σ ) decreasing trend in the alkali metal abundances with decreasing effective temperature, indicative of alkali rainout. As expected from previous work, we also find little evidence for optically thick clouds. With the methane and water abundances, we derive the intrinsic atmospheric metallicity and carbon-to-oxygen ratios. We find in our sample that metallicities are typically subsolar (−0.4 < [ M /H] < 0.1 dex) and carbon-to-oxygen ratios are somewhat supersolar (0.4 < C/O < 1.2), different than expectations from the local stellar population. We also find that the retrieved vertical thermal profiles are consistent with radiative equilibrium over the photospheric regions. Finally, we find that our retrieved effective temperatures are lower than previous inferences for some objects and that some of our radii are larger than expectations from evolutionary models, possibly indicative of unresolved binaries. This investigation and method represent a new and powerful paradigm for using spectra to determine the fundamental chemical and physical processes governing cool brown dwarf atmospheres.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-10-20
Publisher Place United States
Journal Astrophysical Journal
Volume Number 848
Issue Number 2


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