由引力波观测确定超新星的angular momentum分布
Determination of the angular momentum distribution of supernovae from gravitational wave observations
摘要：
国际引力波探测器网络的发展取得了重大进展，如TAMA 300、LIGO、VIRGO和GEO600。对于这些探测器来说，最有希望的引力波来源之一是核心坍缩超新星，特别是在我们的银河系中。最近的模拟核心坍缩超新星，严格地进行了不同的团体，表明波形的功能是由核心的旋转配置文件，如旋转速率和程度的差异旋转之前，核心坍缩。具体地说，已经预测，如果核心以强差旋转进行圆柱旋转，则引力波应变信号中的第二大峰值的符号为负。第二个峰值的符号可能是一个很好的指示器，它为我们提供了关于核心角动量分布的信息，没有引力波信号就看不见。在这里，我们提出了一个数据分析的程序，旨在检测的第二个峰值，使用相干网络分析和估计的检测效率时，超新星是在银河系中心的天空位置。模拟显示，如果银河系中心发生超新星，我们能够在引力波探测器网络的理想条件下确定第二个峰值的符号。
英文摘要：
Significant progress has been made in the development of an international network of gravitational wave detectors, such as TAMA300, LIGO, VIRGO, and GEO600. For these detectors, one of the most promising sources of gravitational waves are core collapse supernovae especially in our Galaxy. Recent simulations of core collapse supernovae, rigorously carried out by various groups, show that the features of the waveforms are determined by the rotational profiles of the core, such as the rotation rate and the degree of the differential rotation prior to core-collapse. Specifically, it has been predicted that the sign of the second largest peak in the gravitational wave strain signal is negative if the core rotates cylindrically with strong differential rotation. The sign of the second peak could be a nice indicator that provides us with information about the angular momentum distribution of the core, unseen without gravitational wave signals. Here we present a data analysis procedure aiming at the detection of the second peak using a coherent network analysis and estimate the detection efficiency when a supernova is at the sky location of the Galactic center. The simulations showed we were able to determine the sign of the second peak under an idealized condition of a network of gravitational wave detectors if a supernova occurs at the Galactic center.
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