Rapid Contraction of a Protostar to the Stage of Quasi-Hydrostatic Equilibrium. I ---The Case of One Solar Mass without Radiation Flow---

Details Rapid Contraction of a Protostar to the Stage of Quasi-Hydrostatic Equilibrium. I ---The Case of One Solar Mass without Radiation Flow--- Rapid Contraction of a Protostar to the Stage of Quasi-Hydrostatic Equilibrium. I ---The Case of One Solar Mass without Radiation Flow---

Jun 1968

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968pthph..39.1448n&link_type=abstract

Progress of Theoretical Physics, Vol. 39, No. 6, pp. 1448-1467

Physics

20

Scientific paper

The evolution of an opaque protostar of one solar mass is investigated up to the onset stage of quasi-hydrostatic equilibrium by solving numerically the hydrodynamic equations of motion. The protostar is assumed to retain spherical symmetry. The dissipation of the energy of mass motion by shock waves is taken into account, but the radiation flow in the protostar is neglected because of the rapidity of the dynamics. It is found that the stellar structure at the onset stage of quasi-hydrostatic equilibrium is insensitive to the initial distributions of density and temperature in the protostar. At this onset stage the star has an isothermal and dense core and a tenuous envelope with a radius of about 200R_&sun;. By the shock wave an outermost envelope having a mass as small as 10^{-4}M_&sun; is ejected from the star.

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