Rapid Contraction of a Protostar to the Stage of Quasi-Hydrostatic Equilibrium. I : The Case of One Solar Mass without Radiation Flow
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概要
- 論文の詳細を見る
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_<xdoi>. By the shock wave an outermost envelope having a mass as small as 10^<-4>M_<xdoi> is ejected from the star.
- 理論物理学刊行会の論文
- 1968-06-25
著者
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Hayashi Chushiro
Department Of Nuclear Science Kyoto University
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Ohyama Noboru
Department Of Nuclear Science Kyoto University
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Ohyama Noboru
Department Of Physics Hiroshima University
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Nakano Takenori
Research Institute For Fundamental Physics Kyoto University
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