论文标题
来自潮汐破坏事件的重力波背景信号
The gravitational wave background signal from tidal disruption events
论文作者
论文摘要
在本文中，我们从潮汐破坏事件（TDES）中得出引力波随机背景。我们专注于星系核中超级质量黑洞（SMBH）发出的主要序列恒星发出的信号，并从位于球形簇中的中间质量黑洞（IMBH）的白色矮人破坏。我们表明，特征应变$ h _ {\ rm c} $对频率的依赖性是由潮汐半径内事件的候选器分布所影响的，并且根据标准假设$ h _ {\ rm c} \ propto f^{ - 1/2} $。这是因为TDE信号是最接近的轨道频率下的重力波爆发。此外，我们将背景特征菌株与即将产生的空间引力波干涉仪的灵敏度曲线进行比较：激光干涉仪太空天线（LISA），Tianqin，Alia，Deci-Hertz强化仪重力仪重力仪重力仪重力观测值（DECIGO）和Big Bang Bang Bang Observer（bbo）。我们发现，BBO在其最低频率覆盖范围内可能仅检测到主序列产生的背景，但对于所有其他仪器来说，它都太弱了。另一方面，带有白色矮人的TDE的背景信号将在AliA范围内，尤其是Decigo和BBO的范围内，而它在Lisa和Tianqin敏感曲线下方。该背景信号检测不仅将为IMBH的存在提供证据，直到红移$ z \ sim 3 $，而且还将告知我们每个星系中的球形簇的数量以及在这些环境中IMBH的职业分数。
In this paper we derive the gravitational wave stochastic background from tidal disruption events (TDEs). We focus on both the signal emitted by main sequence stars disrupted by super-massive black holes (SMBHs) in galaxy nuclei, and on that from disruptions of white dwarfs by intermediate mass black holes (IMBHs) located in globular clusters. We show that the characteristic strain $h_{\rm c}$'s dependence on frequency is shaped by the pericenter distribution of events within the tidal radius, and under standard assumptions $h_{\rm c} \propto f^{-1/2}$. This is because the TDE signal is a burst of gravitational waves at the orbital frequency of the closest approach. In addition, we compare the background characteristic strains with the sensitivity curves of the upcoming generation of space-based gravitational wave interferometers: the Laser Interferometer Space Antenna (LISA), TianQin, ALIA, the DECI-hertz inteferometer Gravitational wave Observatory (DECIGO) and the Big Bang Observer (BBO). We find that the background produced by main sequence stars might be just detected by BBO in its lowest frequency coverage, but it is too weak for all the other instruments. On the other hand, the background signal from TDEs with white dwarfs will be within reach of ALIA, and especially of DECIGO and BBO, while it is below the LISA and TianQin sensitive curves. This background signal detection will not only provide evidence for the existence of IMBHs up to redshift $z\sim 3$, but it will also inform us on the number of globular clusters per galaxy and on the occupation fraction of IMBHs in these environments.
