Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. II ---Evolution of Stellar Cores of Initial Masses 10 and 3M&sun;---

Details Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. II ---Evolution of Stellar Cores of Initial Masses 10 and 3M&sun;--- Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. II ---Evolution of Stellar Cores of Initial Masses 10 and 3M&sun;---

Sep 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970pthph..44..599s&link_type=abstract

Progress of Theoretical Physics, Vol. 44, No. 3, pp. 599-616

Physics

36

Scientific paper

Evolution of stellar cores of initial masses 10 and 3M&sun; is studied from helium-burning phase up to exhaustion of oxygen in the central region of the core. These cores are assumed to have been formed as a result of hydrogen burning of the stars of mass around 30 and 12M&sun;. As discussed in Paper I of this series, hydrogen-rich envelope with an extended surface convection zone is taken into account by replacing it with suitable boundary conditions at the outer edge of the core. For the core of initial mass 10M&sun;, the convection in the envelope is found to become deeper and deeper after a stage near the onset of carbon burning. When there is no neutrino loss, about 4M&sun; of the material in the core has been mixed into the envelope before the exhaustion of oxygen. When there is neutrino loss due to the universal Fermi interaction, on the other hand, amount of mixing is limited after carbon burning phase, because the time-scale of evolution is too short compared with the time-scale of heat transfer. For the core of initial mass 3M&sun;, the mixing begins after oxygen-burning phase. Such a difference in mixing as well as difference in chemical evolution of the stars is discussed.

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