Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. III ---Stellar Core of Initial Mass 1.5M_&sun;---

Details Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. III ---Stellar Core of Initial Mass 1.5M_&sun;--- Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. III ---Stellar Core of Initial Mass 1.5M_&sun;---

Mar 1971

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971pthph..45..761s&link_type=abstract

Progress of Theoretical Physics, Vol. 45, No. 3, pp. 761-775

Physics

49

Scientific paper

As a continuation of the preceding papers of this series, evolution of stellar core of initial mass 1.5 M_&sun; is studied, starting from helium-burning phase. This core is assumed to have been formed as a result of hydrogen burning of the star of mass around 6 M_&sun;. When neutrino loss due to the universal Fermi interaction is taken into account, electrons become degenerate in a central region of the core after exhaustion of helium. In this respect, evolution of our core of mass 1.5 M_&sun; is different from ones of mass greater than 3 M_&sun; which have been studied in the preceding paper of this series. In the phase of contracting carbon-oxygen core with neutrino loss, a surface convection zone in hydrogen-rich envelope penetrates into the core, and the core mass is reduced to 1.07 M_&sun; by mixing. Because of cooling by neutrinos, temperature is maximum in an outlying shell of the core. Then, two carbon-shell flashes take place successively in the outlying shell. Convective zone, which appears in the carbon-oxygen core, does not reach the outer edge of the core. After the carbon-shell flashes, the core is cooled down. Simultaneously, hydrogen-shell burning becomes active, and the convective envelope penetrates into the core. It is suggested that hydrogen is depleted uniformly in the envelope until the star comes to have a helium envelope.

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