论文标题
主要序列星的潮汐破坏-V。破坏的品种
Tidal Disruptions of Main Sequence Stars -- V. The Varieties of Disruptions
论文作者
论文摘要
潮汐破坏事件（TDE），恒星经过非常接近超级黑洞的事件通常被认为是导致恒星完全破坏或直接进入黑洞的事件。在前一种情况下，人们普遍认为，由于相对论的Apsidal进动，即形成紧凑的积聚磁盘，碎片的结合部分迅速“循环”“循环”，并散发出标准化的灯波和光谱。我们在这里表明TDE更多样化，可以根据出色的围师距离$ r_p $将其分为几个不同的类别；我们计算这些类别的相对频率。特别是，由于快速循环化需要$ r_p \ Lessim 10r_g $（$ r_g \ equiv gm _ {\ rm bh}/c^2 $），它只能发生在少数完全干扰的少数情况下，$ \ lyssim 1/4 $，当黑洞具有质量$ m_ _________________________________6时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.分数质量损失$ \ gtrsim 10 \％$的部分中断应以类似于总干扰的比率；对于分数质量损失$ \ gtrsim 50 \％$，费率为$ \ 1/3 $。部分中断 - 当恒星在“空损失 - 锥”状态中演变的角动量发展时，必须在总干扰之前进行整体干扰 - 通过因素$ \ gtrsim o（1）$改变轨道能量。部分干扰的残留物通常远离热平衡。根据SMBH周围恒星簇内的残留物和条件的轨道能量，它可能会在数百年或数千年后返回，并受到完全破坏，或者可能会重新加入恒星群。
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.
