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arXiv 2601.02476astro-ph.HE
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部分潮汐破坏事件的最大重力模型：质量损失、峰值回落率及对恒星属性的依赖

The Maximum Gravity Model for partial Tidal Disruption Events: Mass Loss, Peak Fallback Rate and Dependence on Stellar Properties

Syracuse University（雪城大学）；University of Leeds（利兹大学）

Ananya Bandopadhyay, Eric R. Coughlin, C. J. Nixon

备注：
21 pages, 14 figures, 1 table; ApJ accepted
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AI总结：

本文提出一个分析模型，用于描述部分潮汐破坏事件的峰值回落率、峰值时间及质量损失，通过与水动力学模拟对比，验证了模型在不同恒星属性下的适用性。

摘要：

一颗进入超大质量黑洞（SMBH）潮汐球的恒星可能会部分失去质量，导致部分潮汐破坏事件（TDE）。在这里，我们开发了一个分析模型，用于描述这些事件的属性，包括峰值回落率$\dot{M}_{\rm peak}$、峰值发生时间$t_{\rm peak}$以及从恒星中移除的质量$ΔM$，对于任何恒星和任何与黑洞轨道相关的过近距离。我们将模型预测与1276个主序星部分TDE的水动力学模拟进行了比较，由$10^6 M_\odot$的SMBH执行。模型得出的$t_{\rm peak}$预测与数值模拟在几十个百分点内一致，对于任何恒星质量和年龄都适用。由于自引力对碎片流动力学的影响，$\dot{M}_{\rm peak}$的预测一致性较弱；然而，在大多数考虑的情况下，$\dot{M}_{\rm peak}$的预测与数值模拟在因子$\sim 2-3$范围内一致，对于低质量恒星（$M_\star \lesssim 0.5 M_\odot$）在接近轨道上有较小质量损失的情况下，差异更大。我们表明，由$\sim 10^6M_\odot$SMBH引起的部分TDE光变曲线可以覆盖$\sim 20-100$天的峰值时间尺度，而高质量恒星与高质量SMBH的接近遭遇可以产生更长的峰值时间尺度（$t\gtrsim 1000$天），与一些观测到的暂现源相关。我们的模型为TDE光变曲线和光度函数的分析处方提供了重要进展。

英文摘要：

A star entering the tidal sphere of a supermassive black hole (SMBH) can be partially stripped of mass, resulting in a partial tidal disruption event (TDE). Here we develop an analytical model for properties of these events, including the peak fallback rate, $\dot{M}_{\rm peak}$, the time at which the peak occurs, $t_{\rm peak}$, and the amount of mass removed from the star, $ΔM$, for any star and any pericenter distance associated with the stellar orbit about the black hole. We compare the model predictions to 1276 hydrodynamical simulations of partial TDEs of main-sequence stars by a $10^6 M_\odot$ SMBH. The model yields $t_{\rm peak}$ predictions that are in good agreement (to within tens of percent) with the numerical simulations for any stellar mass and age. The agreement for $\dot{M}_{\rm peak}$ is weaker due to the influence of self-gravity on the debris stream dynamics, which remains dynamically important for partial TDEs; the agreement for $\dot{M}_{\rm peak}$ is, however, to within a factor of $\sim 2-3$ in the majority of cases considered, with larger differences for low-mass stars ($M_\star \lesssim 0.5 M_\odot$) on grazing orbits with small mass loss. We show that partial TDE lightcurves for disruptions caused by $\sim 10^6M_\odot$ SMBHs can span $\sim 20-100$ day peak timescales, whereas grazing encounters of high-mass stars with high-mass SMBHs can yield longer peak timescales ($t\gtrsim 1000$ days), associated with some observed transients. Our model provides a significant step toward an analytical prescription for TDE lightcurves and luminosity functions.

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