Gravitational waves from relativistic neutron-star mergers with microphysical equations of state

被引：88

作者：

Oechslin, R. ^{[1
]}

Janka, H.-T. ^{[1
]}

机构：

[1] Max Planck Inst Astrophys, D-85741 Garching, Germany

来源：

PHYSICAL REVIEW LETTERS | 2007年 / 99卷 / 12期

关键词：

D O I：

10.1103/PhysRevLett.99.121102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The gravitational wave (GW) emission from a set of relativistic neutron-star (NS) merger simulations is analyzed and characteristic signal features are identified. The distinct peak in the GW energy spectrum that is associated with the formation of a hypermassive merger remnant has a frequency that depends strongly on the properties of the nuclear equation of state (EOS) and on the total mass of the binary system, whereas the mass ratio and the NS spins have a weak influence. If the total mass can be determined from the inspiral chirp signal, the peak frequency of the post-merger signal is a sensitive indicator of the EOS.

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