论文标题
GSN 069中潮汐破坏事件与准周期喷发之间可能连接的模型
A model for the possible connection between tidal disruption event and quasi-periodic eruption in GSN 069
论文作者
论文摘要
准周期爆发（QPE）在五个星系的中心发现，在QPE前几年发生的GSN 069中，GSN 069也报告了潮汐破坏事件（TDE）类似事件。我们根据高度偏心的白色视过（WD）的模型来解释这些现象的联系 - $ 10^{4-6} M _ {\ odot} $由山丘机制形成的大量黑洞（MBH）二进制。在该系统中，潮汐诱导的WD的内部振荡可以加热WD包膜，从而诱导潮汐Nova并膨胀WD包膜，WD包膜可以由MBH捕获并形成TDE。偏心轨道中存活的WD的潮汐剥离会产生QPE。我们还将此模型应用于其他四个QPE源。基于估计的后备率，我们发现这些QPE的QPE观察时间之后的剩余时间仅基于我们的简单模型估计约1 - 2年，然后WD将完全中断。我们还表明，在这些QPE来源的最后阶段，积聚率可能高于爱丁顿的增生率。磁盘的光谱能分布的峰值频率停留在软X射线频带（$ \ sim 0.1-1 $ keV）中，这与观察结果一致。
Quasi-periodic eruptions (QPEs) are found in the center of five galaxies, where a tidal disruption event (TDE)-like event is also reported in GSN 069 that happened a couple of years before the QPEs. We explain the connection of these phenomena based on a model of a highly eccentric white-dwarf (WD)-$10^{4-6}M_{\odot}$ massive black hole (MBH) binary formed by the Hill mechanism. In this system, the tidal induced internal oscillation of WD can heat the WD envelope thereby induces the tidal nova and inflates the WD envelope, which can be captured by the MBH and form a TDE. The tidal stripping of the surviving WD in the eccentric orbit can produce the QPEs. We also apply this model to the other four QPE sources. Based on the estimated fallback rate, we find that the remaining time after the QPE-observed time for these QPEs is only around 1-2 years based on our simple model estimation, and then the WD will be fully disrupted. We also show that the accretion rate can be much higher than Eddington accretion rate in final stage of these QPE sources. The peak frequency of spectral energy distribution of disk stays in soft X-ray band ($\sim 0.1-1$ keV), which is consistent with observational results.
