Equation-of-state Dependence of Gravitational Waves in Core-collapse Supernovae
Equation-of-state Dependence of Gravitational Waves in Core-collapse Supernovae
复制标题
核心塌陷超新星中引力波的状态方程依赖性
DOI：
10.3847/1538-4357/ac294c
复制
发表时间：
2021
期刊：
影响因子：
--
通讯作者：
E. O’Connor
中科院分区：
文献类型：
--
作者：
Oliver Eggenberger Andersen;S. Zha;André da Silva Schneider;Aurore Betranhandy;S. Couch;E. O’Connor
引力波（GW）提供了对核心塌陷超新星（CCSNe）中中子星和黑洞诞生地的清晰了解。描述这些致密环境的核状态方程 (EOS) 尚不确定，其规定的变化会影响原中子星 (PNS) 和 CCSN 模拟中的弹跳后动力学，从而影响引力波发射。我们使用 Skyrme 型 EOS 对 CCSNe 进行轴对称模拟，以研究 GW 信号和 PNS 对流区如何受到两个实验可访问的 EOS 参数的影响，（1）核子的有效质量 m ⋆，这对于设置 EOS 的热依赖性至关重要，以及（2）等标量不可压缩模量 K sat。虽然 K sat 几乎没有影响，但由于热压降低，PNS 的收缩速度更快，m ⋆ 值更高，因此引力波的峰值频率具有很强的有效质量依赖性。这些更紧凑的PNS还表现出更多的中微子加热，这会驱动更早的爆炸，并通过撞击PNS的吸积羽流与引力波振幅相关，从而激发振荡。我们研究了引力波的空间起源，并显示了引力波发射的频率径向分布与扰动分析之间的一致性。我们不排除通过 PNS 对流从下方产生超调，作为我们模拟中的另一种中等强度的激励机制。我们还研究了有效质量和旋转的综合影响。在我们所有的模拟中，我们发现了~1250 Hz 附近功率差距的证据；我们调查其起源并报告其对 EOS 的依赖。
Gravitational waves (GWs) provide unobscured insight into the birthplace of neutron stars and black holes in core-collapse supernovae (CCSNe). The nuclear equation of state (EOS) describing these dense environments is yet uncertain, and variations in its prescription affect the proto−neutron star (PNS) and the post-bounce dynamics in CCSN simulations, subsequently impacting the GW emission. We perform axisymmetric simulations of CCSNe with Skyrme-type EOSs to study how the GW signal and PNS convection zone are impacted by two experimentally accessible EOS parameters, (1) the effective mass of nucleons, m ⋆, which is crucial in setting the thermal dependence of the EOS, and (2) the isoscalar incompressibility modulus, K sat. While K sat shows little impact, the peak frequency of the GWs has a strong effective mass dependence due to faster contraction of the PNS for higher values of m ⋆ owing to a decreased thermal pressure. These more compact PNSs also exhibit more neutrino heating, which drives earlier explosions and correlates with the GW amplitude via accretion plumes striking the PNS, exciting the oscillations. We investigate the spatial origin of the GWs and show the agreement between a frequency-radial distribution of the GW emission and a perturbation analysis. We do not rule out overshoot from below via PNS convection as another moderately strong excitation mechanism in our simulations. We also study the combined effect of effective mass and rotation. In all our simulations we find evidence for a power gap near ∼1250 Hz; we investigate its origin and report its EOS dependence.
DOI：
10.3847/2041-8213/ab191a
发表时间：
2018-12
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
D. Radice;V. Morozova;A. Burrows;D. Vartanyan;H. Nagakura
通讯作者：
D. Radice;V. Morozova;A. Burrows;D. Vartanyan;H. Nagakura
影响因子：
5
作者：
M. Szczepańczyk;J. Antelis;M. Benjamin;M. Cavaglià;D. Gondek-Rosińska;T. Hansen;S. Klimenko;M. Mora
通讯作者：
M. Szczepańczyk;J. Antelis;M. Benjamin;M. Cavaglià;D. Gondek-Rosińska;T. Hansen;S. Klimenko;M. Mora