Molecular structure of brown-dwarf disks View Full Text


Ontology type: schema:ScholarlyArticle      Open Access: True


Article Info

DATE

2008-11

AUTHORS

D. S. Wiebe, D. A. Semenov, T. Henning

ABSTRACT

We describe typical features of the chemical composition of proto-planetary disks around brown dwarfs. We model the chemical evolution in the disks around a low-mass T Tauri star and a cooler brown dwarf over a time span of 1 Myr using a model for the physical structure of an accretion disk with a vertical temperature gradient and an extensive set of gas-phase chemical reactions. We find that the disks of T Tauri stars are, in general, hotter and denser than the disks of lower-luminosity substellar objects. In addition, they have more pronounced vertical temperature gradients. The atmospheres of the disks around low-mass stars are more strongly ionized by UV and X-ray radiation, while less dense brown-dwarf disks have higher fractional ionizations in their midplanes. Nevertheless, in both cases, most molecules are concentrated in the so-called warm molecular layer between the ionized atmosphere and cold midplane, where grains with ice mantles are abundant. More... »

PAGES

941-949

Identifiers

URI

http://scigraph.springernature.com/pub.10.1134/s1063772908110103

DOI

http://dx.doi.org/10.1134/s1063772908110103

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1011635812


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