论文标题
超大颗星的旋转
The Rotation of SuperMassive Stars
论文作者
论文摘要
已经提出，质量> 10^5 $ m $ _ \ odot $的超质量星（SMSS）被认为是在Redshifts $ z> 6-7 $上观察到的最极端超级质量黑洞的可能的祖细胞。在这种情况下（“直接崩溃”），SMS以$> 0.1 $ M $ _ \ odot $ yr $^{ - 1} $的价格收益，直到它通过一般相关（GR）不稳定倒塌到黑洞。旋转在形成这种超级质量黑洞种子中起着至关重要的作用。在这种极端的恒星形成情况下，离心屏障显得特别强。此外，旋转会影响SMS对GR的稳定性以及随后的崩溃。特别是，它可能允许在黑洞形成处进行重力波发射和超长的伽马射线爆发，这代表了目前在文献中为存在这种物体提出的主要观察性特征。在这里，我介绍了有关积聚和轮换的SMSS的最新模型，并讨论了该研究行中的一些开放问题和未来的前景。
Supermassive stars (SMSs), with masses $>10^5$ M$_\odot$, have been proposed as the possible progenitors of the most extreme supermassive black holes observed at redshifts $z>6-7$. In this scenario ('direct collapse'), a SMS accretes at rates $>0.1$ M$_\odot$ yr$^{-1}$ until it collapses to a black hole via the general-relativistic (GR) instability. Rotation plays a crucial role in the formation of such supermassive black hole seeds. The centrifugal barrier appears as particularly strong in this extreme case of star formation. Moreover, rotation impacts sensitively the stability of SMSs against GR, as well as the subsequent collapse. In particular, it might allow for gravitational wave emission and ultra-long gamma-ray bursts at black hole formation, which represents currently the main observational signatures proposed in the literature for the existence of such objects. Here, I present the latest models of SMSs accounting for accretion and rotation, and discuss some of the open questions and future prospects in this research line.
