Gravitational wave asteroseismology with fast rotating neutron stars
Gravitational wave asteroseismology with fast rotating neutron stars
复制标题
快速旋转中子星的引力波星震学
DOI：
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发表时间：
2010
期刊：
影响因子：
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通讯作者：
K. Kokkotas
中科院分区：
文献类型：
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作者：
E. Gaertig;K. Kokkotas
在原中子星星的诞生或两颗较老的致密恒星的合并过程中，可能会激发出剧烈的非径向振荡，导致大量的引力辐射的发射[1]。从振荡的中子星探测引力波将允许研究其内部，就像日震学提供有关太阳内部的信息一样。预计在观测数据中识别特定的脉动频率将揭示物质在密度下的真实性质，这是今天任何其他实验都无法探测的。在本文中，我们提出了快速旋转中子星四极f模的模式频率和阻尼时间的新经验关系，扩展了以前处理非旋转情况的研究[2 - 4]。
During the birth of a proto-neutron star or the merging of two older compact stars, violent non-radial oscillations may be excited, resulting in the emission of significant amounts of gravitational radiation [1]. The detection of gravitational waves from oscillating neutron stars will allow the study of their interior, in the same way as helioseismology provides information about the interior of the Sun. It is expected that the identification of specific pulsation frequencies in the observational data will reveal the true properties of matter at densities that cannot be probed today by any other experiment. In this paper, we present new empirical relationships for mode-frequencies and damping times of the quadrupolar f -mode for rapidly rotating neutron stars, extending previous studies which deal with the non-rotating case [2‐4].