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首页> 外文期刊>Physical review, D >Low mass binary neutron star mergers: Gravitational waves and neutrino emission
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Low mass binary neutron star mergers: Gravitational waves and neutrino emission

机译：低质量二元中子星兼并：引力波和中微子排放

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摘要

Neutron star mergers are among the most promising sources of gravitational waves for advanced ground-based detectors. These mergers are also expected to power bright electromagnetic signals, in the form of short gamma-ray bursts, infrared/optical transients powered by r-process nucleosynthesis in neutron-rich material ejected by the merger, and radio emission from the interaction of that ejecta with the interstellar medium. Simulations of these mergers with fully general relativistic codes are critical to understand the merger and postmerger gravitational wave signals and their neutrinos and electromagnetic counterparts. In this paper, we employ the Spectral Einstein Code to simulate the merger of low mass neutron star binaries (two 1.2M(circle dot) neutron stars) for a set of three nuclear-theory-based, finite temperature equations of state. We show that the frequency peaks of the postmerger gravitational wave signal are in good agreement with predictions obtained from recent simulations using a simpler treatment of gravity. We find, however, that only the fundamental mode of the remnant is excited for long periods of time: emission at the secondary peaks is damped on a millisecond time scale in the simulated binaries. For such low mass systems, the remnant is a massive neutron star which, depending on the equation of state, is either permanently stable or long lived (i.e. rapid uniform rotation is sufficient to prevent its collapse). We observe strong excitations of l = 2, m = 2 modes, both in the massive neutron star and in the form of hot, shocked tidal arms in the surrounding accretion torus. We estimate the neutrino emission of the remnant using a neutrino leakage scheme and, in one case, compare these results with a gray two-moment neutrino transport scheme. We confirm the complex geometry of the neutrino emission, also observed in previous simulations with neutrino leakage, and show explicitly the presence of important differences in the neutrino luminosity, disk composition, and outflow properties between the neutrino leakage and transport schemes.
机译：中子星兼并是用于先进地基探测器的最有希望的引力波源。这些合并还期望通过通过合并弹出的中子富含材料的富γ射线突发，红外/光学瞬变为富γ射线突发，红外/光学瞬变的形式发电，以及从该喷射器的相互作用的无线电发射与星际媒体。具有完全一般相对论代码的这些合并的模拟对于了解合并和激活的引力波信号及其中微子和电磁对应物至关重要。在本文中，我们采用光谱爱因斯坦代码来模拟低质量中子星二进制二进制二进制（两个1.2M（圆点）中子恒星）的一组基于核理论，有限的状态的有限温度方程。我们表明，活器重力波信号的频率峰值与使用更简单的重力的初步模拟获得的预测良好。然而，我们发现，只有长时间激励残余物的基本模式：二次峰值的发射在模拟二进制中的毫秒时间尺度上被阻尼。对于这种低质量系统，残余物是巨大的中子明星，其取决于状态的等式，是永久稳定的或长寿命的（即快速均匀旋转足以防止其塌陷）。我们观察到L = 2，M = 2种模式的强烈激发，既是大规模中子星，也以热，震动潮汐臂的形式，在周围的潮汐圆环中。我们使用中性漏贮池方案估计残余物的中性发射，并且在一种情况下，将这些结果与灰色的双力量传输方案进行比较。我们确认中微子发射的复杂几何形状，同时在先前的模拟中观察到中微子泄漏，并明确显示中微子泄漏和运输方案之间的中性亮度，盘组合物和流出性质的重要差异。

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  • 来源
    《Physical review, D》 |2016年第1期|共23页
  • 作者

    Foucart Francois; Haas Roland; Duez Matthew D.; OConnor Evan; Ott Christian D.; Roberts Luke; Kidder Lawrence E.; Lippuner Jonas; Pfeiffer Harald P.; Scheel Mark A.;

  • 作者单位

    Univ Calif Berkeley Lawrence Berkeley Natl Lab 1 Cyclotron Rd Berkeley CA 94720 USA;

    Max Planck Inst Gravitat Phys Albert Einstein Inst D-14476 Golm Germany;

    Washington State Univ Dept Phys &

    Astron Pullman WA 99164 USA;

    N Carolina State Univ Dept Phys Raleigh NC 27695 USA;

    CALTECH Walter Burke Inst Theoret Phys TAPIR MC 350-17 Pasadena CA 91125 USA;

    CALTECH Walter Burke Inst Theoret Phys TAPIR MC 350-17 Pasadena CA 91125 USA;

    Cornell Univ Cornell Ctr Astrophys &

    Planetary Sci Ithaca NY 14853 USA;

    CALTECH Walter Burke Inst Theoret Phys TAPIR MC 350-17 Pasadena CA 91125 USA;

    Univ Toronto Canadian Inst Theoret Astrophys Toronto ON M5S 3H8 Canada;

    CALTECH Walter Burke Inst Theoret Phys TAPIR MC 350-17 Pasadena CA 91125 USA;

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  • 正文语种 eng
  • 中图分类 粒子物理学;场论;
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