发表机构
Swinburne University of Technology; ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav); Monash University（斯威本科技大学; 引力波发现卓越研究中心; 莫纳什大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过137个轴对称核心坍缩超新星模拟，系统探究前身星质量、旋转速率和核态方程对引力波辐射的影响，发现CMF态方程和快速旋转显著改变信号特征，并首次揭示随机扰动可使信噪比变化达62%，同时提出改进的高频模式普适关系校准。
AI 中文摘要
我们模拟了137个轴对称核心坍缩超新星爆炸，以系统研究不同前身星性质、旋转速率和态方程对超新星引力波辐射的影响。我们使用了15颗不同的前身星，质量范围从9.71个太阳质量到36.61个太阳质量，三种态方程和三种旋转速率，模拟持续时间延伸至反弹后5.5秒。我们发现不同态方程之间的引力波辐射存在显著差异，其中CMF态方程产生的引力波振幅较低，并且由于驻立激波不稳定性，低频模式持续时间更长，即使在反弹后约5秒时仍然可见。快速旋转也显著改变了引力波信号，引力波辐射中出现更多可见模式，但由于激波复苏时间较晚，能量较低。我们包含了中微子记忆引起的引力波辐射，并表明对于具有改进低频灵敏度的观测站，它可以显著提高核心坍缩超新星的可探测性。我们提出对高频模式的普适关系进行重新校准，使用对我们波形的拟合，以减少引力波信号后期时间的拟合误差。最后，我们首次研究了随机种子扰动对引力波辐射的影响。我们发现随机扰动可以导致引力波振幅的剧烈变化，并且对于处于激波复苏失败与成功之间边界附近的模型，可以将探测的信噪比改变多达62%。
英文摘要
We simulate 137 axisymmetric core-collapse supernova explosions to systematically investigate the impact of different progenitor properties, rotation rates, and equations of state on the supernova gravitational-wave emission. We use 15 different progenitor stars, with masses ranging from $9.71\,\mathrm{M}_{\odot}$ to $36.61\,\mathrm{M}_{\odot}$, three equations of state, and three rotation rates, with durations extending up to 5.5\,s after bounce. We find substantial differences in the gravitational-wave emission between equations of state, with the CMF equation of state producing lower gravitational-wave amplitudes and a longer low frequency mode due to the standing accretion shock instability that remains visible even at $\sim5$\,s post bounce. Rapid rotation also significantly alters the gravitational-wave signal, with more visible modes in the gravitational-wave emission, and lower energies due to later shock revival times. We include the gravitational-wave emission due to neutrino memory, and show it can significantly improve the detectability of core-collapse supernovae for observatories with improved low frequency sensitivity. We propose a recalibration of universal relations for the high frequency mode, using fits to our waveforms, that reduces the fit error at late times in the gravitational-wave signal. Finally, we investigate, for the first time, the impact of random seed perturbations on the gravitational-wave emission. We find that stochastic perturbations can produce dramatic variations in gravitational-wave amplitude, and can alter the signal-to-noise ratio of a detection by as much as 62\% for models close to the boundary between failed and successful shock revival.
