论文标题
恒星的潮汐破坏半径和潮汐破坏事件中的峰值增生率的简单准确的处方
A simple and accurate prescription for the tidal disruption radius of a star and the peak accretion rate in tidal disruption events
论文作者
论文摘要
在潮汐破坏事件（TDE）中，一颗被超级质量黑洞（SMBH）摧毁的星星使SMBH的研究能够研究。我们建议，通过将SMBH潮汐场（包括数值因子）等于恒星中的最大重力场，可以准确估算恒星完全被SMBH（定义的$ r _ {\ rm t，c} $）完全破坏的距离。我们证明该定义准确地重现了关键$β_ {\ rm c} = r _ {\ rm t}/r _ {\ rm t，c} $，其中$ r _ {\ rm t} = r _ {\ star} \ left（m _ {\ bullet}/m _ {\ star} \ right）^{1/3} $是标准的潮汐半径，带有$ r _ {\ star} $ and $ m _ {\ star} $ sentelr and ass and Mass and $ m _ _ {在各个年龄段，可以合理地通过$β_ {\ rm c} \ simeq \ left [ρ_{\ rm c}/（4ρ_{\ star}）\ right] 密度。我们还计算了峰值的后备率和时间，即后备率达到峰值，与流体动力学模拟找到了极好的一致性，并表明部分中断半径 - 任何质量从星星中成功释放的距离为$β__{\ rm partial} \ rm partial} \ simeq 4^{ - 1/1/3} \ simeq 0.6 $ simeq 0.6 $。对于给定的恒星和SMBH种群，该模型产生，例如，部分TDE的比例，TDE的峰值光度分布以及直接捕获的恒星的数量。
A star destroyed by a supermassive black hole (SMBH) in a tidal disruption event (TDE) enables the study of SMBHs. We propose that the distance within which a star is completely destroyed by a SMBH, defined $r_{\rm t, c}$, is accurately estimated by equating the SMBH tidal field (including numerical factors) to the maximum gravitational field in the star. We demonstrate that this definition accurately reproduces the critical $β_{\rm c} = r_{\rm t}/r_{\rm t, c}$, where $r_{\rm t} = R_{\star}\left(M_{\bullet}/M_{\star}\right)^{1/3}$ is the standard tidal radius with $R_{\star}$ and $M_{\star}$ the stellar radius and mass and $M_{\bullet}$ the SMBH mass, for multiple stellar progenitors at various ages, and can be reasonably approximated by $β_{\rm c} \simeq \left[ρ_{\rm c}/(4ρ_{\star})\right]^{1/3}$, where $ρ_{\rm c}$ ($ρ_{\star}$) is the central (average) stellar density. We also calculate the peak fallback rate and time at which the fallback rate peaks, finding excellent agreement with hydrodynamical simulations, and also suggest that the partial disruption radius -- the distance at which any mass is successfully liberated from the star -- is $β_{\rm partial} \simeq 4^{-1/3} \simeq 0.6$. For given stellar and SMBH populations, this model yields, e.g., the fraction of partial TDEs, the peak luminosity distribution of TDEs, and the number of directly captured stars.
