大质量恒星中的原磁星和黑洞形成
Protomagnetar and black hole formation in high-mass stars
摘要：
使用轴对称模拟耦合特殊相对论MHD，一个近似的后牛顿引力势和两个时刻中微子运输，我们显示不同的路径形成的原磁星或恒星质量的黑洞。原型恒星核心中产生类星体的比例取决于几个因素的组合，其中祖先恒星的结构和特定角动量的分布可能是最重要的。随着恒星核的内爆，我们也得到了超新星般的爆炸驱动的中微子加热和流体动力学不稳定性或磁旋转效应的核心的大质量恒星。在后一种情况下，高度准直，温和的相对论流出产生。我们发现，在一个相当长的后坍缩阶段（持续>~ 1秒）黑洞可能形成的情况下，成功的和失败的supernovalike爆炸。一个基本的趋势是，具有特定角动量的核心比标准的一维恒星演化计算得到的角动量小，形成黑洞（并最终形成黑洞）。作为补充，原磁星来自恒星核心，其特定角动量的标准分布是从原型恒星演化计算中获得的，包括磁矩和中等到大的质量损失率。
英文摘要：
Using axisymmetric simulations coupling special relativistic MHD, an approximate post-Newtonian gravitational potential and two-moment neutrino transport, we show different paths for the formation of either protomagnetars or stellar mass black holes. The fraction of prototypical stellar cores which should result in collapsars depends on a combination of several factors, among which the structure of the progenitor star and the profile of specific angular momentum are probably the foremost. Along with the implosion of the stellar core, we also obtain supernova-like explosions driven by neutrino heating and hydrodynamic instabilities or by magneto-rotational effects in cores of high-mass stars. In the latter case, highly collimated, mildly relativistic outflows are generated. We find that after a rather long post-collapse phase (lasting >~ 1 sec) black holes may form in cases both of successful and failed supernovalike explosions. A basic trend is that cores with a specific angular momentum smaller than that obtained by standard, one-dimensional stellar evolution calculations form black holes (and eventually collapsars). Complementary, protomagnetars result from stellar cores with the standard distribution of specific angular momentum obtained from prototypical stellar evolution calculations including magnetic torques and moderate to large mass loss rates.
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