Gravitational waves from hot young rapidly rotating neutron stars
Gravitational waves from hot young rapidly rotating neutron stars
复制标题
DOI：
10.1103/physrevd.58.084020
复制
发表时间：
1998-04
影响因子：
5
通讯作者：
B. Owen;L. Lindblom;C. Cutler;B. Schutz;A. Vecchio;N. Andersson
中科院分区：
文献类型：
--
作者：
B. Owen;L. Lindblom;C. Cutler;B. Schutz;A. Vecchio;N. Andersson
引力辐射导致年轻的快速旋转的中子星的r模不稳定。这种不稳定性预计会通过引力辐射发射带走恒星的大部分角动量，使恒星以大约100赫兹的速度旋转。在本文中，我们用一种简单的方式模拟了中子星在长达一年的自旋下降阶段的不稳定性和演化的发展。这使我们能够预测由此产生的引力波形的一般特征。我们发现，当LIGO和室女座引力波探测器达到“增强”的灵敏度水平时，在室女座星系团中形成的中子星可以被探测到，如果发展出近最佳的数据分析技术，其幅度信噪比可能高达约8。我们还分析了由中子星形成产生的r模辐射在整个宇宙中产生的引力波的随机背景。假设很大一部分中子星出生时的自旋频率接近其最大值，在20赫兹到1千赫的范围内，这个随机背景的能量密度大约是宇宙闭合密度的10^(−9)。这种辐射也应该可以被“高级”LIGO探测到。
Gravitational radiation drives an instability in the r-modes of young rapidly rotating neutron stars. This instability is expected to carry away most of the angular momentum of the star by gravitational radiation emission, leaving a star rotating at about 100 Hz. In this paper we model in a simple way the development of the instability and evolution of the neutron star during the year-long spindown phase. This allows us to predict the general features of the resulting gravitational waveform. We show that a neutron star formed in the Virgo cluster could be detected by the LIGO and VIRGO gravitational wave detectors when they reach their “enhanced” level of sensitivity, with an amplitude signal-to-noise ratio that could be as large as about 8 if near-optimal data analysis techniques are developed. We also analyze the stochastic background of gravitational waves produced by the r-mode radiation from neutron-star formation throughout the universe. Assuming a substantial fraction of neutron stars are born with spin frequencies near their maximum values, this stochastic background is shown to have an energy density of about 10^(−9) of the cosmological closure density, in the range 20 Hz to 1 kHz. This radiation should be detectable by “advanced” LIGO as well.