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The evolution of very low mass starsThe results of numerical evolutionary calculations for stars with masses in the range of 0.01-0.10 solar mass are presented. The stellar models by which these stars are followed from the early stages of contraction through deuterium burning to the very late stages of degenerate cooling at ages comparable to that of the Galaxy are described, and the methodology used to investigate the major uncertainties in the input physics are discussed. It is found that, for brown dwarfs with masses substantially below the end of the hydrogen-burning main sequence, the evolution of the effective temperature and bolometric luminosity are fairly well determined, despite the residual uncertainties in the input physics. In particular, the evolution is remarkably insensitive to the choice of the atmospheric opacity law at low temperatures and to the amount of mismatch in specific entropy across the stellar envelope. The minimum mass for a star to attain main-sequence status is moderately sensitive to the assumed input physics, particularly the surface boundary conditions.
Document ID
19870039546
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Nelson, L. A.
(Massachusetts Inst. of Tech. Cambridge, MA, United States)
Rappaport, S. A.
(Massachusetts Inst. of Tech. Cambridge, MA, United States)
Joss, P. C.
(MIT Cambridge, MA, United States)
Date Acquired
August 13, 2013
Publication Date
December 1, 1986
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 311
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
87A26820
Funding Number(s)
CONTRACT_GRANT: NGL-22-009-638
CONTRACT_GRANT: NSG-7643
CONTRACT_GRANT: NSF AST-84-19834
CONTRACT_GRANT: NAS5-24441
Distribution Limits
Public
Copyright
Other

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