Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae
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DOI：
10.1093/mnras/stx618
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发表时间：
2016-07
影响因子：
4.8
通讯作者：
H. Andresen;B. Mueller;E. Mueller;H. J. M. Astrophysics;Garching;Physik Dept.;Tum;Queen's University of Belfast;Monash University
中科院分区：
文献类型：
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作者：
H. Andresen;B. Mueller;E. Mueller;H. J. M. Astrophysics;Garching;Physik Dept.;Tum;Queen's University of Belfast;Monash University
我们提出了引力波（GW）信号的预测，从四个3D多群中微子流体动力学模拟的核心坍缩超新星的祖先与11.2 Msun，20 Msun，和27 Msun。GW的排放在爆炸前阶段强烈依赖于后冲击流是否占主导地位的常设吸积激波不稳定性（SASI）或对流，并从2D模型有很大的不同。SASI活动通过增益层中的不对称质量运动和与原中子星星（PNS）的非共振耦合产生低于250 Hz的强信号分量。对流和SASI占主导地位的模型显示GW发射高于250 Hz，但幅度大大低于2D。这是由于PNS表面中的高频l=2运动的不同激发机制，其主要由3D中的PNS对流激发。与2D相比，由于更小的下流速度和在下流中缺乏高频可变性，在3D中由增益层中的质量运动对高频表面g模式的共振激发被抑制。在爆炸20 Msun模型中，激波复活导致增强的低频发射，由于在PNS对流区的对流涡的首选尺度的变化。对两个频段的预期过剩功率的估计表明，第二代探测器将只能探测到非常近的事件，但第三代探测器可以在~10 kpc的距离上区分SASI和对流主导的模型。
We present gravitational wave (GW) signal predictions from four 3D multi-group neutrino hydrodynamics simulations of core-collapse supernovae of progenitors with 11.2 Msun, 20 Msun, and 27 Msun. GW emission in the pre-explosion phase strongly depends on whether the post-shock flow is dominated by the standing accretion shock instability (SASI) or convection and differs considerably from 2D models. SASI activity produces a strong signal component below 250 Hz through asymmetric mass motions in the gain layer and a non-resonant coupling to the proto-neutron star (PNS). Both convection- and SASI-dominated models show GW emission above 250 Hz, but with considerably lower amplitudes than in 2D. This is due to a different excitation mechanism for high-frequency l=2 motions in the PNS surface, which are predominantly excited by PNS convection in 3D. Resonant excitation of high-frequency surface g-modes in 3D by mass motions in the gain layer is suppressed compared to 2D because of smaller downflow velocities and a lack of high-frequency variability in the downflows. In the exploding 20 Msun model, shock revival results in enhanced low-frequency emission due to a change of the preferred scale of the convective eddies in the PNS convection zone. Estimates of the expected excess power in two frequency bands suggests that second-generation detectors will only be able to detect very nearby events, but that third-generation detectors could distinguish SASI- and convection-dominated models at distances of ~10 kpc.