The evolution of very low mass stars

摘要: The results of numerical evolutionary calculations for stars with masses in the range 0.01-0.10 solar mass are presented. stellar models by which these followed from early stages contraction through deuterium burning to very late degenerate cooling at ages comparable that Galaxy described, and methodology used investigate major uncertainties input physics discussed. It is found that, brown dwarfs substantially below end hydrogen-burning main sequence, evolution effective temperature bolometric luminosity fairly well determined, despite residual physics. In particular, remarkably insensitive choice atmospheric opacity law low temperatures amount mismatch specific entropy across envelope. minimum a star attain main-sequence status moderately sensitive assumed physics, particularly surface boundary conditions. 58 references.