冷却在触发超大质量中子星坍缩中的重要性
Importance of cooling in triggering the collapse of hypermassive neutron stars
摘要：
双中子星（NSNS）的螺旋和合并可以导致超大质量中子星（HMNS）的形成。当HMNS由于中微子冷却和/或由于引力波（GW）发射的离心支持而失去热压力时，和/或差旋转的磁破坏，它将坍缩成黑洞。为了评估冲击引起的热压力和冷却的重要性，我们采用了一个理想化的状态方程，并通过后期螺旋，合并和HMNS的形成，占冷却在全GR进行NSNS模拟。我们表明，热压力有助于显着的支持HMNS对崩溃和热冷却加速其“延迟”崩溃。我们的模拟明确地表明，冷却可以导致一个热的超大质量中子星合并后形成的双中子星的灾难性崩溃。因此，冷却物理学是重要的，包括在NSNS合并计算，以准确地确定HMNS残留物的寿命，并提取有关NS状态方程，冷却机制，酒吧的不稳定性和B-场的信息，从全球变暖发射的瞬态阶段之前BH的形成。
英文摘要：
The inspiral and merger of a binary neutron star (NSNS) can lead to the formation of a hypermassive neutron star (HMNS). As the HMNS loses thermal pressure due to neutrino cooling and/or centrifugal support due to gravitational wave (GW) emission, and/or magnetic breaking of differential rotation it will collapse to a black hole. To assess the importance of shock-induced thermal pressure and cooling, we adopt an idealized equation of state and perform NSNS simulations in full GR through late inspiral, merger, and HMNS formation, accounting for cooling. We show that thermal pressure contributes significantly to the support of the HMNS against collapse and that thermal cooling accelerates its "delayed" collapse. Our simulations demonstrate explicitly that cooling can induce the catastrophic collapse of a hot hypermassive neutron star formed following the merger of binary neutron stars. Thus, cooling physics is important to include in NSNS merger calculations to accurately determine the lifetime of the HMNS remnant and to extract information about the NS equation of state, cooling mechanisms, bar instabilities and B-fields from the GWs emitted during the transient phase prior to BH formation.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
