论文标题
主要序列星的潮汐破坏-IV。相对论效应和对黑洞质量的依赖性
Tidal disruptions of main sequence stars -- IV. Relativistic effects and dependence on black hole mass
论文作者
论文摘要
我们使用一套完全相对论的流体动力学模拟，应用于具有逼真的内部密度曲线的主要序列恒星，我们检查了各种黑洞质量（$ 10^{5} \ leq m _ {\ leq m _ {\ rm bh}/\ rm bh}/\ mathrm {m Mathrm {m} $ {恒星质量（$ 0.3 \ leq m _ {\ star} /\ mathrm {m} _ {\ odot} \ leq 3 $）作为较大的$ $ m _ {\ rm bh} $导致更强的相对论效应。对于固定的$ m _ {\ star} $，AS $ m _ {\ rm bh} $增加，最大距离距离距离产生完全中断的比率（$ \ Mathcal {r} _ {\ rm t} $）迅速上升，成为纽顿的newtonian vor $ m m _ 5 \ times10^{7}〜{\ rm m} _ \ odot $，而恒星碎片的能量宽度与牛顿预测的完全干扰的比率急剧下降，从而导致$ m _ {\ rm bh} = 5 \ t $ \ f tese $ f tese 10^7〜 \ od \ od \ od \ od \ od。我们发现，对于部分中断，对于较大的$ M _ {\ rm bh} $而言，给定比例与$ \ Mathcal {rm t} $给定比率的分数残余质量更高。这些结果有几个含义。由于$ m _ {\ rm bh} $在$ \ sim 10^7〜 {\ rm m} _ \ odot $上方增加，因此与直接捕获的竞争抑制了用于完全中断的横截面。但是，部分的横截面比率仅取决于$ m _ {\ rm bh} $。对碎片能宽度的相对论校正延迟了峰值返回率的时间，并降低了峰值回报率的幅度。对于$ m _ {\ rm bh} \ gtrsim 10^7〜 {\ rm m} _ \ odot $，$ m _ {\ rm bh} $ - 完全中断横截面的依赖性，峰值返回率和时间的影响和时间比新顿动力学对相对效应更大。
Using a suite of fully relativistic hydrodynamic simulations applied to main-sequence stars with realistic internal density profiles, we examine full and partial tidal disruptions across a wide range of black hole mass ($10^{5}\leq M_{\rm BH}/\mathrm{M}_{\odot}\leq 5\times 10^{7}$) and stellar mass ($0.3 \leq M_{\star} /\mathrm{M}_{\odot}\leq 3$) as larger $M_{\rm BH}$ leads to stronger relativistic effects. For fixed $M_{\star}$, as $M_{\rm BH}$ increases, the ratio of the maximum pericenter distance yielding full disruptions ($\mathcal{R}_{\rm t}$) to its Newtonian prediction rises rapidly, becoming triple the Newtonian value for $M_{\rm BH} = 5\times10^{7}~{\rm M}_\odot$, while the ratio of the energy width of the stellar debris for full disruptions to the Newtonian prediction decreases steeply, resulting in a factor of two correction at $M_{\rm BH} = 5 \times 10^7~{\rm M}_\odot$. We find that for partial disruptions, the fractional remnant mass for a given ratio of the pericenter to $\mathcal{R}_{\rm t}$ is higher for larger $M_{\rm BH}$. These results have several implications. As $M_{\rm BH}$ increases above $\sim 10^7~{\rm M}_\odot$, the cross section for complete disruptions is suppressed by competition with direct capture. However, the cross section ratio for partial to complete disruptions depends only weakly on $M_{\rm BH}$. The relativistic correction to the debris energy width delays the time of peak mass-return rate and diminishes the magnitude of the peak return rate. For $M_{\rm BH} \gtrsim 10^7~{\rm M}_\odot$, the $M_{\rm BH}$-dependence of the full disruption cross section and the peak mass-return rate and time is influenced more by relativistic effects than by Newtonian dynamics.
