Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. III : Stellar Core of Initial Mass 1.5M&xodoi;

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概要

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• As a continuation of the preceding papers of this series, evolution of stellar core of initial mass 1.5M&xodoi; 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 6M&xodoi;. 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 1.5M&xodoi; is different from ones of mass greater than 3M&xodoi; 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 1.07M&xodoi; 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, dose 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.

• 理論物理学刊行会の論文
• 1971-03-25

著者

• Sugimoto Daiichiro

  Institute Of Earth Science And Astronomy College Of General Education University Of Tokyo

関連論文

• Mixing between Stellar Envelope and Core in Advanced Phases of Evolution. III : Stellar Core of Initial Mass 1.5M&xodoi;

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