论文标题
快速喷射是在高质量重力波事件中区分黑洞和中子星的潜在方法
Fast ejecta as a potential way to distinguish black holes from neutron stars in high-mass gravitational-wave events
论文作者
论文摘要
在中子明星质量范围（例如GW190425）中，高质量引力波事件最近已被Ligo/Pirgo探测器检测到。如果两个二进制组件的质量落在中子星质量范围内，则该系统通常被归类为二元中子星系，尽管检测到的重力波信号可能太嘈杂了，无法清楚地确定二进制中的高质量组件的中子星性质，并且将黑洞的二进制组件和规则排除在黑洞中，以实现此类事件。我们在这里表明，具有非常庞大的中子星级初级的高质量二进制中子恒星合并，接近最大质量限制，$ m_1 \ gtrsim 2.2 \，m_ \ odot $，从主星的旋转中产生快速的动态质量弹出。通过模拟黑洞的合并 - 完全相同的质量和旋转的独立星系，我们表明这些快速喷射完全不存在，如果主要是一个黑洞。此外，我们发现这两个系统几乎都留下了几乎相同数量的重子质量，而黑洞并未立即吸收。这意味着这两个系统都可能具有由残留磁盘引起的可比电磁源发射。因此，合并的快速喷射具有将中子星与高质量合并中的黑洞区分开的潜力，尽管这些喷射可能在观察上检测到挑战。
High-mass gravitational-wave events in the neutron-star mass range, such as GW190425, have recently started to be detected by the LIGO/Virgo detectors. If the masses of the two binary components fall in the neutron-star mass range, such a system is typically classified as a binary neutron-star system, although the detected gravitational-wave signal may be too noisy to clearly establish a neutron-star nature of the high-mass component in the binary and rule out a black hole--neutron star system for such an event. We here show that high-mass binary neutron-star mergers with a very massive neutron-star primary close to the maximum-mass limit, $m_1 \gtrsim 2.2 \, M_\odot$, produce fast dynamical mass ejecta from the spin-up of the primary star at merger. By simulating the merger of black hole--neutron star systems of exactly the same masses and spins, we show that these fast ejecta are entirely absent, if the primary is instead a black hole. In addition, we find that both systems leave almost identical amounts of baryon mass behind, which is not immediately accreted by the black hole. This implies that both systems will likely have comparable electromagnetic afterglow emission stemming from the remnant disk. Hence, fast ejecta at merger have the potentialto distinguish neutron stars from black holes in high-mass mergers, although these ejecta may be challenging to detect observationally.
