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High mass planets and low mass stars

Stevenson, D. J. (1986) High mass planets and low mass stars. In: Astrophysics of brown dwarfs. Cambridge University Press , Cambridge, pp. 218-232. ISBN 9780521323376. http://resolver.caltech.edu/CaltechAUTHORS:20130724-152608478

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Abstract

There are three main ingredients in brown dwarf theoretical models: (i) The equation of state; (ii) The entropy equation, which relates the internal and atmospheric thermodynamic states; and (iii) The atmospheric boundary condition (the infrared opacity). It is argued that the first two ingredients are very well understood. The opacity is less well understood and the major unresolved problem. Simple scaling laws are described and discussed for the relationships between luminosity (L), mass, opacity and age (t), assuming no thermonuclear energy sources. In the limit of extreme degeneracy, L ∝ t^(-1.25). However, detectable brown dwarfs (including VB8B) are still significantly contracting (i.e. actual radius ~10% larger than the zero temperature limit). As a consequence, dlnL/dlnt ~ -1.0 to -1.1 at this epoch for VB8B. Large opacity increases the effect of non-degeneracy. Complicating factors in brown dwarf evolution (super- or sub-adiabaticity, Debye cooling, freezing, differentiation, variable opacity) are discussed but only the latter two seem like to be important.


Item Type:Book Section
ORCID:
AuthorORCID
Stevenson, D. J.0000-0001-9432-7159
Additional Information:© 1986 Cambridge University Press.
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Caltech Division of Geological and Planetary Sciences 4288
Record Number:CaltechAUTHORS:20130724-152608478
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20130724-152608478
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39566
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:20 Sep 2013 20:29
Last Modified:24 Nov 2015 01:52

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