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arXiv 2001.03502astro-ph.HEastro-ph.GAastro-ph.SR
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主序星的潮汐破裂-- II。全潮破裂特征的模拟方法和恒星质量依赖性

Tidal disruptions of main sequence stars -- II. Simulation methodology and stellar mass dependence of the character of full tidal disruptions

Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble

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19 pages, 10 figures, 3 tables, accepted for publication in ApJ, Supersedes arXiv:1907.11883
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摘要：

这是一系列论文中的第二篇，介绍了恒星潮汐破裂的完全广义相对论模拟结果，其中恒星的初始状态是现实的主序星模型。在第一篇论文（论文I）中，我们概述了这一计划，并讨论了我们工作的主要观测意义。在这里，我们描述了我们的计算方法，并提供详细的全面破坏的结果，专注于恒星质量依赖的质量$10^{6}\rm{M}_{\odot}$的黑洞的结果。我们考虑八个不同的恒星质量，从$0.15~{\rm M}_\odot$到$10~{\rm M}_\odot$。我们发现，相对于传统的数量级估计$r_{\rm t}$，低质量恒星的物理潮汐半径（$M_{\star} \lesssim 0.7~ {\rm M}_\odot$）大百分之几十，而对于高质量恒星（$M_{\star} \gtrsim1~ {\rm M}_\odot$），它是小的2- 2.5倍。传统的碎片能量范围估计是$\approx 1.4\times$对低质量恒星来说太大，但对高质量恒星来说是一个$\sim 2$太小的因子;此外，高质量恒星的能量分布有明显的翼。对于所有的恒星经历潮汐遭遇，我们发现，质量损失持续许多恒星振动时间，因为黑洞的潮汐引力竞争与瞬时恒星引力在恒星的表面，直到恒星已经达到了距离黑洞$\sim O(10)r_{\rm t}$。

英文摘要：

This is the second in a series of papers presenting the results of fully general relativistic simulations of stellar tidal disruptions in which the stars' initial states are realistic main-sequence models. In the first paper (Paper I), we gave an overview of this program and discussed the principal observational implications of our work. Here we describe our calculational method and provide details about the outcomes of full disruptions, focusing on the stellar mass dependence of the outcomes for a black hole of mass $10^{6}\rm{M}_{\odot}$. We consider eight different stellar masses, from $0.15~{\rm M}_\odot$ to $10~{\rm M}_\odot$. We find that, relative to the traditional order-of-magnitude estimate $r_{\rm t}$, the physical tidal radius of low-mass stars ($M_{\star} \lesssim 0.7~ {\rm M}_\odot$) is larger by tens of percent, while for high-mass stars ($M_{\star} \gtrsim1~ {\rm M}_\odot$) it is smaller by a factor 2--2.5. The traditional estimate of the range of energies found in the debris is $\approx 1.4\times$ too large for low-mass stars, but is a factor $\sim 2$ too small for high-mass stars; in addition, the energy distribution for high-mass stars has significant wings. For all stars undergoing tidal encounters, we find that mass-loss continues for many stellar vibration times because the black hole's tidal gravity competes with the instantaneous stellar gravity at the star's surface until the star has reached a distance from the black hole $\sim O(10)r_{\rm t}$.

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