Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. II : 10, 10^2, 10^3 and 10^4 Solar Masses without Radiation Flow
スポンサーリンク
概要
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The collapse of opaque protostars of 10, 10^2, 10^3 and 10^4Mxodoi is computed up to the onset stage of quasi-hydrostatic equilibrium in the same way as for 1Mxodoi in a previous paper. The protostars are assumed to retain spherical symmetry. The dissipation of mass motion energy by shock waves is taken into account, but the energy flow in the protostars is ne-glected for simplicity. It is found that a mass ejected from the surface by the shock wave is negligibly small for the protostars of 1 and 10Mxodoi, while it amounts to 10 or 15 per cent of the total mass for the protostars of 10^2, 10^3 and 10^4Mxodoi. The structure of the stars of 1 and 10Mxodoi at the onset stage of quasi-hydrostatic equilibrium is found to be homologous. However, this homology does not extend to the stars of greater masses, in which radiation pressure is important.
- 理論物理学刊行会の論文
- 1970-03-25
著者
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Hayashi Chushiro
Department Of Nuclear Science Kyoto University
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Ohyama Noboru
Faculty Of Engineering Shizuoka University
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Nakano Takenori
Research Institute For Fundamental Physics Kyoto University
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