中子星的角动量和作为超新星窗口的黑洞
The Angular Momenta of Neutron Stars and Black Holes as a Window on Supernovae
摘要：
现在很清楚，超新星的一个子集显示出喷流的证据，并被观察到伽马射线暴。大质量恒星端点的角动量分布提供了一种罕见的手段来限制核心坍缩爆炸中中心引擎的性质。与超大质量黑洞不同，X射线双星系统中恒星质量黑洞的自旋几乎不受吸积的影响，并且准确地反映了出生时的自旋。现在，我们已经用两种独立的X射线光谱技术测量了少量恒星质量的黑洞角动量。相比之下，旋转动力的行星会随着时间的推移通过磁制动而自旋下降，但现在已经估计出了适度数量的出生自旋周期。对于正则和极端中子星参数，统计检验强烈表明黑洞和中子星的角动量分布是明显不同的。在核心坍缩超新星的流行模型的背景下，角动量分布与通常在具有喷流的GRB类超新星中产生的黑洞以及通常在角动量太小而无法通过磁流体动力学过程产生喷流的超新星中产生的中子星是一致的。可能中子星在初始时具有高自旋，在超新星事件后不久迅速自旋下降，但现有的机制可能与某些观测到的脉冲星性质不一致。
英文摘要：
It is now clear that a subset of supernovae display evidence for jets and are observed as gamma-ray bursts. The angular momentum distribution of massive stellar endpoints provides a rare means of constraining the nature of the central engine in core-collapse explosions. Unlike supermassive black holes, the spin of stellar-mass black holes in X-ray binary systems is little affected by accretion, and accurately reflects the spin set at birth. A modest number of stellar-mass black hole angular momenta have now been measured using two independent X-ray spectroscopic techniques. In contrast, rotation-powered pulsars spin-down over time, via magnetic braking, but a modest number of natal spin periods have now been estimated. For both canonical and extreme neutron star parameters, statistical tests strongly suggest that the angular momentum distributions of black holes and neutron stars are markedly different. Within the context of prevalent models for core-collapse supernovae, the angular momentum distributions are consistent with black holes typically being produced in GRB-like supernovae with jets, and with neutron stars typically being produced in supernovae with too little angular momentum to produce jets via magnetohydrodynamic processes. It is possible that neutron stars are imbued with high spin initially, and rapidly spun-down shortly after the supernova event, but the available mechanisms may be inconsistent with some observed pulsar properties.
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