相对论性超大质量中子星的磁转不稳定性
Magnetorotational instability in relativistic hypermassive neutron stars
摘要：
差异旋转超大质量中子星（HMNS）是中子星双星合并过程中形成的亚稳态天体。HMNS最终坍缩成黑洞是产生预期伴随着短伽马射线暴发射的物理条件的关键因素。我们研究了磁场对HMNS的影响，通过在广义相对论磁流体力学中进行三维模拟。特别是，我们提供了直接的证据，在HMNS内部的磁旋转不稳定性（MRI）的发生。在这些系统的模拟中，首次观察到快速生长和空间周期性结构形成的特征与其他系统中MRI产生的通道流的特征相似。此外，增长最快的模式的增长时间和波长的提取和比较成功的分析预测。磁共振成像作为一种重要的机制出现，在HMNS的寿命期间放大磁场，加速其坍缩为黑洞。这里提供的证据表明，磁共振成像实际上可以在HMNS中发展，这可能对中子星双星合并的结果及其与短伽马射线暴的联系产生深远的影响。
英文摘要：
A differentially rotating hypermassive neutron star (HMNS) is a metastable object which can be formed in the merger of neutron-star binaries. The eventual collapse of the HMNS into a black hole is a key element in generating the physical conditions expected to accompany the launch of a short gamma-ray burst. We investigate the influence of magnetic fields on HMNSs by performing three-dimensional simulations in general-relativistic magnetohydrodynamics. In particular, we provide direct evidence for the occurrence of the magnetorotational instability (MRI) in HMNS interiors. For the first time in simulations of these systems, rapidly-growing and spatially-periodic structures are observed to form with features like those of the channel flows produced by the MRI in other systems. Moreover, the growth time and wavelength of the fastest-growing mode are extracted and compared successfully with analytical predictions. The MRI emerges as an important mechanism to amplify magnetic fields over the lifetime of the HMNS, whose collapse to a black hole is accelerated. The evidence provided here that the MRI can actually develop in HMNSs could have a profound impact on the outcome of the merger of neutron-star binaries and on its connection to short gamma-ray bursts.
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