论文标题
主要序列星的潮汐破坏-III。部分破坏特征的恒星质量依赖性
Tidal disruptions of main sequence stars -- III. Stellar mass dependence of the character of partial disruptions
论文作者
论文摘要
在本系列中的第三本书中，我们继续研究通过非旋转$ 10^{6}〜\ rm {m} _ \ odot $ supermassive Black Hole的潮汐破坏事件。在这里，我们关注部分破坏结果的出色质量依赖性。随着相遇变得较弱，碎屑质量越来越集中在能量分布的外边缘附近。结果，质量后备率可以大大偏离$ t^{ - 5/3} $ powerlaw，更像是一个峰值，尾巴下降为$ t^{ - p} $，带有$ p \ simeq2-5 $。幸存的残留物沿着前进方向旋转，并且比同一质量的主要序列星更热。它们的特定轨道能为$ \ simeq10^{ - 3} \ times $碎片的$，但在黑洞电位方面，这两种迹象的特异性动量都接近原始恒星的动量。即使对于强烈的遭遇，残余物的速度相对于黑洞的潜在$ \ Lessim 300 $ km s $^{ - 1} $，因此它们无法进入银河系凸起。最深切地绑定到黑洞的残余物经历了第二次潮汐破坏事件。如果他们没有热放松，它们将被完全破坏。
In this paper, the third in this series, we continue our study of tidal disruption events of main-sequence stars by a non-spinning $10^{6}~\rm{M}_\odot$ supermassive black hole. Here we focus on the stellar mass dependence of the outcomes of partial disruptions. As the encounter becomes weaker, the debris mass is increasingly concentrated near the outer edges of the energy distribution. As a result, the mass fallback rate can deviate substantially from a $t^{-5/3}$ power-law, becoming more like a single peak with a tail declining as $t^{-p}$ with $p\simeq2-5$. Surviving remnants are spun-up in the prograde direction and are hotter than main sequence stars of the same mass. Their specific orbital energy is $\simeq10^{-3}\times$ that of the debris, but of either sign with respect to the black hole potential, while their specific angular momentum is close to that of the original star. Even for strong encounters, remnants have speeds at infinity relative to the black hole potential $\lesssim 300$ km s$^{-1}$, so they are unable to travel far out into the galactic bulge. The remnants most deeply bound to the black hole go through a second tidal disruption event upon their first return to pericenter; if they have not thermally relaxed, they will be completely disrupted.
