Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity

Details Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...296..502d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 296, Sept. 15, 1985, p. 502-513.

Statistics

Computation

184

Brown Dwarf Stars, Main Sequence Stars, Stellar Evolution, Stellar Luminosity, Stellar Mass, Thermonuclear Reactions, Computational Astrophysics, Hertzsprung-Russell Diagram, Mass To Light Ratios, Opacity

Scientific paper

The hydrogen burning minimum mass (HBMM) is determined for solar composition by performing some numerical computations. Pre-main sequence evolution is followed for masses down to 0.04 solar mass, from initial models having central temperatures of 200,000 K, through deuterium burning, until either stable hydrogen burning is reached or the object has cooled down to roughly 10 to the -5th solar luminosity. The opacities are interpolated among the recent opacity tables by Alexander, Johnson, and Rypma (1983), which include a number of important molecules below 4000 K and grain formation below 1500 K. The HBMM turns out to be slightly smaller than predicted with Co and Stewart (1970) opacities, but mainly displays a luminosity ten times smaller. A physical interpretation of this result is presented, and the number of brown dwarfs expected to be detectable near the sun is discussed.

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