The evolution of protostars. II - The hydrostatic core

摘要: We compute the structure and evolution of a protostellar core as problem stellar interiors. Novel techniques are introduced to account for dynamical addition mass follow strikingly disparate thermal responses in different parts star. Early accretion process, deep interior behaves very nearly adiabatically while newly accreted material settles with sharp loss heat. With onset deuterium burning, an inner convection zone develops. Its requires special treatment, which involves rule analogous ''Maxwell's construction'' theory nonideal gases. present numerical results from two evolutionary calculations that begin distributions specific entropy. The sequences converge rapidly time, justifying posteriori our assumption final insensitive detailed mechanism formation core. one model until reaches 1 M/sub sun/. At point, we terminate rapid motion star onto Hayashi track. has radius 4.69 R/sub sun/ luminosity 6.20 L/sub when it begins homologous contraction down convective