Tidal disruption events (TDEs), events in which a star passes very close to a supermassive black hole, are generally imagined as leading either to the star's complete disruption or to its passage directly into the black hole. In the former case it is widely believed that in all cases the bound portion of the debris quickly "circularizes" due to relativistic apsidal precession, i.e., forms a compact accretion disk, and emits a flare of standardized lightcurve and spectrum. We show here that TDEs are more diverse and can be grouped into several distinct categories on the basis of stellar pericenter distance $r_p$; we calculate the relative frequency of these categories. In particular, because rapid circularization requires $r_p \lesssim 10r_g$ ($r_g \equiv GM_{\rm BH}/c^2$), it can happen in only a minority of total disruptions, $\lesssim 1/4$ when the black hole has mass $M_{\rm BH} = 10^6 M_\odot$. For larger pericenter distances, $10 < r_p/r_g < 27$ (for $M_{\rm BH}=10^6M_\odot$), main sequence stars are completely disrupted, but the bound debris orbits are highly eccentric and possess semimajor axes $\sim 100\times$ the scale of the expected compact disk. Partial disruptions with fractional mass-loss $\gtrsim 10\%$ should occur with a rate similar to that of total disruptions; for fractional mass-loss $\gtrsim 50\%$, the rate is $\approx 1/3$ as large. Partial disruptions -- which must precede total disruptions when the stars' angular momenta evolve in the "empty loss-cone" regime -- change the orbital energy by factors $\gtrsim O(1)$. Remnants of partial disruptions are in general far from thermal equilibrium. Depending on the orbital energy of the remnant and conditions within the stellar cluster surrounding the SMBH, it may return after hundreds or thousands of years and be fully disrupted, or it may rejoin the stellar cluster.

中文翻译：

---

主序星的潮汐干扰。五、中断的种类

潮汐瓦解事件 (TDE)，即恒星非常接近超大质量黑洞的事件，通常被认为会导致恒星完全瓦解或直接进入黑洞。在前一种情况下，人们普遍认为，在所有情况下，由于相对论的顶点进动，碎片的结合部分会迅速“圆化”，即形成致密的吸积盘，并发出标准化光曲线和光谱的耀斑。我们在这里展示了 TDE 更加多样化，可以根据恒星周心距离 $r_p$ 分为几个不同的类别；我们计算这些类别的相对频率。特别是，因为快速循环需要 $r_p \lesssim 10r_g$ ($r_g \equiv GM_{\rm BH}/c^2$)，所以它只会发生在少数总中断中，$\lesssim 1/4$ 当黑洞的质量为 $M_{\rm BH} = 10^6 M_\odot$。对于较大的周心距离，$10 < r_p/r_g < 27$（对于$M_{\rm BH}=10^6M_\odot$），主序星完全被打乱，但束缚碎片轨道高度偏心并具有半长轴$\sim 100\times$ 预期光盘的规模。部分质量损失 $\gtrsim 10\%$ 的部分中断应该以类似于总中断的速率发生；对于分数质量损失 $\gtrsim 50\%$，比率是 $\approx 1/3$ 大。部分中断——当恒星的角动量在“空损失锥”状态下演化时，必须先于完全中断——通过因子 $\gtrsim O(1)$ 改变轨道能量。部分破坏的残余物通常远离热平衡。