On the structure of tidally disrupted stellar debris streams
On the structure of tidally disrupted stellar debris streams
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潮汐破坏的恒星碎片流的结构
DOI：
10.1093/mnras/stw770
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发表时间：
2016
影响因子：
4.8
通讯作者：
Coughlin E
中科院分区：
文献类型：
--
作者：
Coughlin E
潮汐分裂事件(TDE)--恒星被超大质量黑洞的巨大引力场摧毁--将恒星转变为潮汐般的碎屑流。这种碎片的性质最终决定了潮汐破坏事件(TDEs)的可观测特征。在这里，我们推导了一个简单的，自相似的解决方案的泥石流产生的泥石流的速度剖面，并表明该解与数值结果非常符合。利用这一自相似解，我们计算了流径向密度分布的解析近似表达式。我们证明了存在一个临界绝热指数，它随位置的变化而变化，在这个临界绝热指数之上(下)，气流对引力碎裂是不稳定的(稳定的)。我们还计算了加热和冷却对稳定性判据的影响。
A tidal disruption event (TDE) – when a star is destroyed by the immense gravitational field of a supermassive black hole – transforms a star into a stream of tidally shredded debris. The properties of this debris ultimately determine the observable signatures of tidal disruption events (TDEs). Here we derive a simple, self-similar solution for the velocity profile of the debris streams produced from TDEs, and show that this solution agrees extremely well with numerical results. Using this self-similar solution, we calculate an analytic, approximate expression for the radial density profile of the stream. We show that there is a critical adiabatic index that varies as a function of position along the stream above (below) which the stream is unstable (stable) to gravitational fragmentation. We also calculate the impact of heating and cooling on this stability criterion.