Instability of Synchronized Binary Neutron Stars in the First Post-Newtonian Approximation of General Relativity : Astrophysics and Relativity
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概要
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We investigate the stability property of binary neutron stars (BNSs) just before the merging in the first post-Newtonian(PN) approximation. Stability analysis is performed making use of equilibrium configurations for synchronized BNSs which are obtained by the numerical scheme developed in a previous paper NSs are modeled by means of the polytropic equation of state with the polytropic exponent Γ=2 and 3. From numerical calculations, we find that as in the Newtonian case, in the PN approximation, the secular instability will occur for synchronized BNSs at a critical angular velocity Ω_<crit> before the surfaces of the two stars come into contact. The PN correction changes not only the gravitational attraction force between two NSs, but also the configuration of each NS of a binary system As a result,Ω_<crit> in the PN approximation is 〜10-15 % larger than that in the Newtonian case for a NS of mass M_<ADM>〜14M_<odot;> radius r_A〜10-15km The implication of this property to the orbital evolution of BNSs just before merging is discussed.
- 理論物理学刊行会の論文
- 1996-08-25
著者
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Sakka Makiko
Graduate School Of Bioresources Mie Univ.
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Shibata M
Univ. Tokyo Tokyo Jpn
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Shibata Masaru
Department Of Agricultural Chemistry Kyoto University:(present)asahi Kasei Chemicals Industry Co. Lt
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SHIBATA Masaru
Department of Earth and Space Science Faculty of Science, Osaka University
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SHIBATA Masaru
Graduate School of Arts and Sciences, University of Tokyo
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