Disequilibrium chemistry in a brown dwarf's atmosphere: Carbon monoxide in Gliese 229B

Research output: Contribution to journalArticle

52 Citations (Scopus)

Abstract

The distribution of CO in Gliese 229B's atmosphere reveals how disequilibrium processes establish the atmospheric composition. The CO abundance derived from its spectral signature exceeds the equilibrium value by several orders of magnitude. Our investigation of the source for CO considers disequilibrium mechanisms common to planetary atmospheres and concludes that the CO abundance is sensitive to atmospheric dynamics. Convection is not required to explain the observed abundance; instead, the vertical transport rate at ∼6 bars may be similar to that in planetary stratospheres.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume519
Issue number1 PART 2
StatePublished - Jul 1 1999
Externally publishedYes

Fingerprint

carbon monoxide
disequilibrium
chemistry
atmospheres
atmosphere
atmospheric composition
planetary atmosphere
planetary atmospheres
atmospheric dynamics
spectral signatures
stratosphere
convection
rate
distribution

Keywords

  • Convection
  • Planets and satellites: general
  • Stars: atmospheres
  • Stars: individual (Gliese 229B)
  • Stars: low-mass, brown dwarfs

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Disequilibrium chemistry in a brown dwarf's atmosphere : Carbon monoxide in Gliese 229B. / Griffith, Caitlin; Yelle, Roger.

In: Astrophysical Journal, Vol. 519, No. 1 PART 2, 01.07.1999.

Research output: Contribution to journalArticle

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AB - The distribution of CO in Gliese 229B's atmosphere reveals how disequilibrium processes establish the atmospheric composition. The CO abundance derived from its spectral signature exceeds the equilibrium value by several orders of magnitude. Our investigation of the source for CO considers disequilibrium mechanisms common to planetary atmospheres and concludes that the CO abundance is sensitive to atmospheric dynamics. Convection is not required to explain the observed abundance; instead, the vertical transport rate at ∼6 bars may be similar to that in planetary stratospheres.

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