Evolution of Close Neutron Star Binaries : Astrophysics and Relativity

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概要

• 論文の詳細を見る

• We have calculated the evolution of neutron star binaries towards the coalescence driven by gravitational radiation. The hydrodynamical effects as well as the general relativistic effects are important in the final phase. All corrections up to post^<2.5>-Newtonian order and the tidal effect are included in the orbital motion. The star is approximated using a simple Newtonian stellar model called the affine star model. Stellar spins and angular momentum are assumed to be aligned. We have shown how the internal stellar structure affects the stellar deformation, variations of the spins,and the orbital motion of the binary Just before contact. The gravitational wave, radiated from the last few revolutions, significantly depends on the stellar structure.

• 理論物理学刊行会の論文
• 1996-11-25

著者

• Kojima Yasuaki

  Graduate School Of Engineering Hiroshima University

• KOJIMA Yasufumi

  Department of Physics, Tokyo Metropolitan University

• Kojima Y

  Department Of Physics Hiroshima University

• Kojima Yasufumi

  Department Of Physics Hiroshima University

• OGAWAGUTI Wataru

  Department of Physics, Tokyo Metropolitan University

• Ogawaguti Wataru

  Department Of Physics Tokyo Metropolitan University

• Kashiv Y.

  Advanced Science Research Center Japan Atomic Energy Agency

• KOJIMA Yasufumi

  Department of Physics, Hiroshima University

• KOJIMA Yasufumi

  Department of Physics, University of Wales

• Ogawaguchi Wataru

  Department of Physics, Tokyo Metropolitan University

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