Chapter 8 Efficiency of Angular Momentum Transfer by Shear Instability : Part II Formation Processes of Protostars : Origin of the Solar System
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概要
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In order to calculate the rate of angular momentum transfer by the shear instability, we use perturbation theory. We obtain the lowest order of the flux of the angular momentum, solving the linear order as well as the second order perturbation equations. The differentially rotating cylinder with isentropic and polytropic equation of state is investigated for the sake of simplicity. The angular momentum is found to be transferred effectively near the corotation point where the phase velocity of the unstable mode is equal to the rotation velocity of the cylinder. Using the results we estimate the angular momentum transfer rate in the solar nebula.
- 理論物理学刊行会の論文
- 1989-03-10
著者
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SEKIYA Minoru
Department of Applied Physics, Tokyo Institute of Technology
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Miyama Shoken
Department Of Physics Kyoto Unvi
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Miyama Shoken
Department Of Physics Kyoto Univeristy
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Sekiya Minoru
Department Of Earth And Planetary Sciences Faculty Of Sciences 33 Kyushu University
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Sekiya Minoru
Department Of Applied Physics Tokyo Institute Of Technology
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Shoken M.
National Astronomical Observatory
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SEKIYA Makoto
Department of Physics, Kyoto University
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SEKIYA Minoru
Department of Physics, Kyoto University
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SEKIYA Minoru
Department of Earth and Planetary Sciences, Faculty of Sciences 33, Kyushu University
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