Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III ---Stars of 0.05, 1.0 and 20M&sun; with Energy Flow by Radiation and Convection---

Details Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III ---Stars of 0.05, 1.0 and 20M&sun; with Energy Flow by Radiation and Convection--- Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III ---Stars of 0.05, 1.0 and 20M&sun; with Energy Flow by Radiation and Convection---

Apr 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970pthph..43..942n&link_type=abstract

Progress of Theoretical Physics, Vol. 43, No. 4, pp. 942-964

Physics

51

Scientific paper

The evolution of collapsing protostars of 0.05, 1 and 20M&sun; is studied with computations which include radiative as well as convective energy flow, which has been entirely neglected in previous papers I and II. It is found that, when a shock wave which has been generated at the center reaches the outermost layers, the protostars flare up suddenly. The protostar of 1M&sun; increases its luminosity from 5 × 10-4 L&sun; to a peak value 6 × 103 L&sun; in a period of the order of 10 days. This peak value depends scarcely on the initial conditions. After the flare-up, a convective region grows inwards from the surface and the luminosity is kept at 1 × 103 L&sun; by convection until the star finally reaches a stage of wholly gravitational equilibtium. The luminosity at this stage is found to be very sensitive to the stellar mass, being 8L&sun; and 5 × 104 L&sun; for the protostars of 0.05 and 20M&sun;. respectively. These computed values of the luminosity are high enough to cover the observations of infrared objects.

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