The evolution of protostars. I - Global formulation and results

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Abstract

A new formulation for the problem of protostar evolution is developed on the basis of a method that involves the division of the global problem into a set of more manageable subproblems. Jump conditions of the radiative accretion shock which joins the hydrostatic mass-gaining core to the dynamic inner cloud envelope are derived. Standard integration schemes yield the high accuracy needed to resolve complex spatial structures which span many orders of magnitude in density and temperature. It is shown that a 1-solar-mass protostar ends its main accretion phase moderately high up in the H-R diagram; this star begins its pre-main-sequence phase of quasi-static contraction on a convective Hayashi track.

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