Thermal Instability of Hydrogen-Burning Shell in Very Massive Stars

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概要

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• The one-zone model has been modified to include the nuclear energy sources and Sackmann's geometrical measure m_s. The deviation of physical quantities from the equilibrium values for entropy perturbations are analytically obtained mainly in terms of m_s and the exponent of the temperature in the nuclear energy production rate n. The conditions that the entropy perturbations grow are: 1) m_s<0.4 and n≳3 and 2) m_s≳2 and n≳14 for the hydrogenburning shell and electron scattering, if we neglect radiation pressures. In the first case, the increase of the temperature in the shell, the decrease of the position of the shell, and the increase of the shell density are induced by the increase of entropy, whereas the second case of thermal instability agrees with the current theory. A mechanism for beta Cephei pulsations is suggested concerning the first case of thermal instability.Thermal instabilityHydrogen-burning shellsMassive starsbeta Cephei stars

• 東北大学の論文
• 1981-06-10

著者

• Arimoto Nobuo

  Astronomical Institute Faculty Of Science Tohoku University

• Takeuti Mine

  Astronomical Institute, Tohoku University

• Takeuti Mine

  Astronomical Institute Tohoku University

• Takeuti M

  Dept. Of Astronomy Tohoku University

• TANAKA Yasuo

  Faculty of Education, Ibaraki University

• Tanaka Yasuo

  Faculty Of Education Ibaraki University

• TAKEUTI M

  Dept. of Astronomy, Tohoku University

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