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---

Details 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--- 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---

Mar 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970pthph..43..672n&link_type=abstract

Progress of Theoretical Physics, Vol. 43, No. 3, pp. 672-683

Physics

6

Scientific paper

The collapse of opaque protostars of 10, 10^2, 10^3 and 10^4M&sun; is computed up to the onset stage of quasi-hydrostatic equilibrium in the same way as for 1M&sun; 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&sun;, while it amounts to 10 or 15 per cent of the total mass for the protostars of 10^2, 10^3 and 10^4M&sun;. The structure of the stars of 1 and 10M&sun; 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.

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