Prog. Theor. Phys. Vol. 43 No. 3 (1970) pp. 672-683
Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. II
— 10, 102, 103 and 104 Solar Masses without Radiation Flow
Research Institute for Fundamental Physics, Kyoto University, Kyoto
*Faculty of Engineering, Shizuoka University, Hamamatsu, Shizuoka
**Department of Physics, Kyoto University, Kyoto
(Received October 21, 1969)
The collapse of opaque protostars of 10, 102, 103 and 104M⊙ is computed up to the onset stage of quasi-hydrostatic equilibrium in the same way as for 1M⊙ 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 neglected 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 10M⊙, while it amounts to 10 or 15 per cent of the total mass for the protostars of 102, 103 and 104M⊙. The structure of the stars of 1 and 10M⊙ 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.
DOI : 10.1143/PTP.43.672
- C. Hayashi and T. Nakano, Prog. Theor. Phys. 34 (1965), 754[PTP].
- C. Hayashi, Ann. Rev. Astron. Astrophys. 4 (1966), 171.
- T. Hattori, T. Nakano and C. Hayashi, Prog. Theor. Phys. 42 (1969), 781[PTP].
- T. Nakano, N. Ohyama and C. Hayashi, Prog. Theor. Phys. 39 (1968), 1448[PTP].
- R. D. Richtmyer, Difference Methods for Initial-Value Problems (Interscience Publishers, Inc., New York, 1957).
- S. Narita, T. Nakano and C. Hayashi, Prog. Theor. Phys. 41 (1969), 856[PTP].
Citing Article(s) :
Progress of Theoretical Physics Vol. 43 No. 4 (1970) pp. 942-964
Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III
Shinji Narita, Takenori Nakano and Chushiro Hayashi
Progress of Theoretical Physics Supplement No.70 (1981) pp. 54-76
Fundamental Processes in Star Formation