Evolution of a Super-Massive Star in a Dense Stellar System
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概要
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The evolution of a Super-Massive Star (SMS) in a dense stellar system is investigated. As the SMS contracts, the dissipation of the stellar kinetic energy via drag force in the SMS increases and bemomes greater than the critical luminosity L_<cr&ft; of the SMS. Then, the SMS does not contract further. In this stage, the SMS adjusts itself automatically to maintain its luminosity close to the Eddington limit L_<cr&ft; by expansion or contraction. Through this control, rather regular luminosity variations can be expected in the order of several months. On the other hand, the collisions among the stars in the stellar system contribute to the sudden luminosity variations by about one collision per year or so. The stars trapped in the SMS sink rapidly toward the center of the SMS and form a high density stellar system where most stars may disintegrate into gas by frequent collisions among themselves and form a small SMS of mass 〜10^6m_⦿ within the large SMS of mass 〜10^8m_⦿
- 理論物理学刊行会の論文
- 1978-09-25
著者
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Hara Tetsuya
Research Institute For Fundamental Physics Kyoto University
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HARA Takashi
Institute of Physics, College of Arts and Science University of Tokyo : Courant Institute of Mathematical Sciences, New York University
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Hara Tetsuya
Research Center for Nuclear Physics, Osaka. University
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