The flare produced when a star is tidally disrupted by a supermassive black hole holds potential as a diagnostic of both the black hole mass and the star mass. We propose a new method to realize this potential based upon a physical model of optical/UV light production in which shocks near the apocenters of debris orbits dissipate orbital energy, which is then radiated from that region. Measurement of the optical/UV luminosity and color temperature at the peak of the flare leads directly to the two masses. The black hole mass depends mostly on the temperature observed at peak luminosity, while the mass of the disrupted star depends mostly on the peak luminosity. We introduce {\sc TDEmass}, a method to infer the black hole and stellar masses given these two input quantities. Using {\sc TDEmass}, we find, for 21 well-measured events, black hole masses between $5\times 10^5$ and $10^7 M_\odot$ and disrupted stars with initial masses between 0.6 and $13M_\odot$. An open-source {\sc python}-based tool for {\sc TDEmass} is available at this https URL.

中文翻译：

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测量潮汐干扰事件的恒星和黑洞质量

当一颗恒星被超大质量黑洞潮汐干扰时产生的耀斑具有作为黑洞质量和恒星质量的诊断的潜力。我们提出了一种基于光学/紫外光产生物理模型来实现这种潜力的新方法，其中碎片轨道顶点附近的冲击会耗散轨道能量，然后从该区域辐射出轨道能量。对耀斑峰值处的光学/紫外线光度和色温的测量直接导致了两个质量。黑洞质量主要取决于峰值光度时观察到的温度，而被破坏恒星的质量主要取决于峰值光度。我们介绍了 {\sc TDEmass}，这是一种在给定这两个输入量的情况下推断黑洞和恒星质量的方法。使用 {\sc TDEmass}，我们发现，对于 21 个测量良好的事件，黑洞质量在 $5\times 10^5$ 和 $10^7 M_\odot$ 之间，以及初始质量在 0.6 和 $13M_\odot$ 之间的被破坏的恒星。此 https URL 提供了基于 {\sc python} 的用于 {\sc TDEmass} 的开源工具。