Darwin-Riemann Problems in Newtonian Gravity
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概要
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In this paper, we have reviewed the present status of the theory of equilibrium configurations of compact binary star systems in Newtonian gravity. Evolutionary processes of compact binary star systems due to gravitational wave emission can be divided into three stages according to the time scales and configurations. The evolution is quasi-stationary until a merging process starts, since the time scale of the orbital change due to gravitational wave emission is longer than the orbital period. In this stage, equilibrium sequences can be applied to evolution of compact binary star systems. Along the equilibrium sequences, there appear several critical states where some instability sets in or configuration changes drastically. We have discussed relations among these critical points and have stressed the importance of the mass overflow as well as the dynamical instability of orbital motions. Concerning the equilibrium sequences of binary star systems, we have summarized classical results of incompressible ellipsoidal configurations. Recent results of compressible binary star systems obtained by the ellipsoidal approximation and by numerical computations have been shown and discussed. It is important to note that numerical computational solutions to exact equations show that compressibility may lead realistic neutron star binary systems to mass overflows instead of dynamical disruptions for a wide range of parameters.
- 理論物理学刊行会の論文
- 2000-01-31
著者
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ERIGUCHI Yoshiharu
Department of Earth Science and Astronomy College of General Education, University of Tokyo
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Eriguchi Yoshiharu
Department Of Earth Science And Astronomy University Of Tokyo
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Eriguchi Yoshiharu
Department Of Earth Science And Astronomy College Of General Education University Of Tokyo
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Eriguchi Yoshiharu
Department Of Earth Science And Astronomy Graduate School Of Arts And Science University Of Tokyo
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URYU Koji
SISSA
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URYU Koji
Department of Physics, University of Wisconsin-Milwaukee
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ERIGUCHI Yoshiharu
Department of Earth Science and Astronomy Graduate School of Arts and Science, University of Tokyo
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- Dumb-Bell-Shape Equilibria and Mass-Shedding Pear-Shape of Selfgravitating Incompressible Fluid
- Gravothermal Aspects in Evolution of the Stars and the Universe
- New Equilibrium Sequences Bifurcating from Maclaurin Sequence
- Bifurcation and Fission of Three Dimensional, Rigidly Rotating and Self-Gravitating Polytropes
- Equation of Motion and a Possibility of Snapping of a Free Cosmic String Loop : Astrophysics and Relativity
- Darwin-Riemann Problems in Newtonian Gravity
- Stable Numerical Method in Computation of Stellar Evolution
- Another Equilibrium Sequence of Self-Gravitating and Rotating Incompressible Fluid
- Possible Evolutionary Transition from Rapidly Rotating Neutron Stars to Strange Stars Due to Spin-Down(Astrophysics and Relativity)
- Rapidly Rotating and Fully General Relativistic Polytropes
- Gravitational Waves from the Merger of Binary Neutron Stars in a Fully General Relativistic Simulation
- General Relativistic Irrotational Binary
- Concave Hamburger Equilibrium of Rotating Bodies