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Author Shibata, Masaru ♦ Taniguchi, Keisuke ♦ Nakamura, Takashi
Source CiteSeerX
Content type Text
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Subject Domain (in DDC) Computer science, information & general works ♦ Data processing & computer science
Subject Keyword Binary Neutron Star ♦ Innermost Stable Circular Orbit ♦ General Relativity ♦ Post Newtonian Approximation ♦ Omega Isco ♦ Following Conclusion ♦ Angular Velocity ♦ Isco Omega Isco ♦ Binary Becomes ♦ Post Newtonian ♦ Recent Study ♦ Stiff Equation ♦ First Pn Correction ♦ Binary Orbit ♦ Newtonian Case ♦ Tidal Effect ♦ Several Level ♦ Latter One ♦ Present Result
Abstract In this paper, we present results obtained from our recent studies on the location of the innermost stable circular orbit (ISCO) for binary neutron stars (BNSs) in several levels of post Newtonian (PN) approximations. We reach the following conclusion at present: (1) even in the Newtonian case, there exists the ISCO for binary of sufficiently stiff equation of state (EOS). If the mass and the radius of each star are fixed, the angular velocity at the ISCO\Omega ISCO is larger for softer EOS: (2) when we include the first PN correction, there appear roughly two kinds of effects. One is the effect to the self-gravity of each star of binary and the other is to the gravity acting between two stars. Due to the former one, each star of binary becomes compact and the tidal effect is less effective. As a result,\Omega ISCO tends to be increased. On the other hand, the latter one has the property to destabilize the binary orbit, and\Omega ISCO tends to be decreased. If we take into account b...
Educational Role Student ♦ Teacher
Age Range above 22 year
Educational Use Research
Education Level UG and PG ♦ Career/Technical Study