Stellar Tidal Disruption Events with Abundances and Realistic Structures (STARS): Library of Fallback Rates
Stellar Tidal Disruption Events with Abundances and Realistic Structures (STARS): Library of Fallback Rates
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DOI：
10.3847/1538-4357/abc489
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发表时间：
2020-07
期刊：
影响因子：
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通讯作者：
J. Law-Smith;D. Coulter;J. Guillochon;B. Mockler;E. Ramirez-Ruiz
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作者：
J. Law-Smith;D. Coulter;J. Guillochon;B. Mockler;E. Ramirez-Ruiz
我们提出了 STARS 库，这是一个潮汐破坏事件 (TDE) 模拟网格，经过插值，可以为任意恒星质量、恒星年龄和撞击参数的主序星提供黑洞的质量回退率 (dM/dt)。我们使用一维恒星演化代码来构建具有精确恒星结构和化学丰度的恒星，然后使用亥姆霍兹状态方程在三维自适应网格流体动力学代码中以前所未有的分辨率进行潮汐破坏模拟：恒星直径上的细胞数量从 131 到 524 个。回退率插值库可在 GitHub (github.com/jamielaw-smith/STARS_library) 上获取，版本 1.0.0 已存档在 Zenodo 上；人们可以在库中查询任何恒星质量、恒星年龄和撞击参数。我们为重要的破坏量 ( ) 提供了新的拟合公式，作为恒星质量、恒星年龄和撞击参数的函数。这些量中的每一个都随恒星质量和恒星年龄而显着变化，但我们能够将所有模拟简化为仅依赖于恒星结构的单一关系，其特征在于单个参数 和影响参数 β。我们还发现，一般来说，更集中的恒星具有更陡的 dM/dt 上升斜率和更浅的衰变斜率。对于相同的 ΔM，dM/dt 形状随恒星质量显着变化，这有望仅根据 TDE 光曲线确定恒星特性。 dM/dt 形状在很大程度上取决于恒星结构和一定程度上的恒星质量，这意味着使用该库拟合 TDE 提供了更好的机会来确定破碎恒星和黑洞的性质。
We present the STARS library, a grid of tidal disruption event (TDE) simulations interpolated to provide the mass fallback rate (dM/dt) to the black hole for a main-sequence star of any stellar mass, stellar age, and impact parameter. We use a one-dimensional stellar evolution code to construct stars with accurate stellar structures and chemical abundances, then perform tidal disruption simulations in a three-dimensional adaptive-mesh hydrodynamics code with a Helmholtz equation of state, in unprecedented resolution: from 131 to 524 cells across the diameter of the star. The interpolated library of fallback rates is available on GitHub (github.com/jamielaw-smith/STARS_library) and version 1.0.0 is archived on Zenodo; one can query the library for any stellar mass, stellar age, and impact parameter. We provide new fitting formulae for important disruption quantities ( ) as a function of stellar mass, stellar age, and impact parameter. Each of these quantities varies significantly with stellar mass and stellar age, but we are able to reduce all of our simulations to a single relationship that depends only on stellar structure, characterized by a single parameter , and impact parameter β. We also find that, in general, more centrally concentrated stars have steeper dM/dt rise slopes and shallower decay slopes. For the same ΔM, the dM/dt shape varies significantly with stellar mass, promising the potential determination of stellar properties from the TDE light curve alone. The dM/dt shape depends strongly on stellar structure and to a certain extent stellar mass, meaning that fitting TDEs using this library offers a better opportunity to determine the nature of the disrupted star and the black hole.