论文标题
快速积累超大质量的星星：最终质量的可靠确定
Rapidly accreting supermassive stars: reliable determination of the final mass
论文作者
论文摘要
超级质量的黑洞可能通过直接崩溃而形成，并以祖细胞为祖细胞（SMS）。在这种情况下，SMS在> 0.1 msun/yr> 0.1 msun造成的增值，直到由于一般相关（GR）的不稳定性而倒入巨大的黑洞种子。但是，由于现有的数值模拟会产生不同的结果，因此崩溃发生的确切质量尚不清楚。在这里，该问题是通过分析解决的，可以从头开始，可靠地确定GR不稳定性的发作点，对于给定的静水结构。我们将其一般形式的径向脉动的相对论方程式应用于已经发布的静液压基因模型。我们表明，与先前的索赔相比，在原子冷却的光环中形成的球形SMS质量不能超过500 000 msun。另一方面，可以在直接崩溃的替代版本中达到超过此极限的质量，最高为10^6 msun。我们的方法可用于测试GR流体动力学恒星演化代码的一致性。
Supermassive black holes might form by direct collapse, with a supermassive star (SMS) as progenitor. In this scenario, the SMS accretes at > 0.1 Msun/yr until it collapses into a massive black hole seed due to the general-relativistic (GR) instability. However, the exact mass at which the collapse occurs is not known, as existing numerical simulations give divergent results. Here, this problem is addressed analytically, which allows for ab initio, reliable determination of the onset point of the GR instability, for given hydrostatic structures. We apply the relativistic equation of radial pulsations in its general form to the hydrostatic GENEC models already published. We show that the mass of spherical SMSs forming in atomically cooled haloes cannot exceed 500 000 Msun, in contrast to previous claims. On the other hand, masses in excess of this limit, up to 10^6 Msun, could be reached in alternative versions of direct collapse. Our method can be used to test the consistency of GR hydrodynamical stellar evolution codes.
