论文标题
中间质量黑洞潮汐剥离白矮人
Tidal Stripping of a White Dwarf by an Intermediate-Mass Black Hole
论文作者
论文摘要
在将白色矮人（WD）的灵感化为中间质量黑洞（〜10^{2-5} m_sun）期间，发射引力波（GWS）和电磁（EM）辐射。一旦怪异的轨道的折缘半径接近潮汐半径，WD将被潮汐剥离。这些被剥离的质量的积聚会产生EM辐射。怀疑最近发现的新型瞬变类型，即准周期性喷发和快速的超X射线爆发，可能源自此类系统。对这些耀斑进行建模需要预测WD中剥离的质量量以及对积聚磁盘的质量供应细节。我们运行流体动力学模拟以研究剥离质量的轨道参数依赖性。我们发现我们的结果与剥离质量的分析估计与z^{5/2}成正比的分析估计，其中z是WD过度填充其瞬时的Roche lobe的过度深度。计算了剥离质量的相应后备率，这对于解释候选EM源中的单个耀斑光曲线可能很有用。我们进一步计算了WD在其灵感过程中的长期质量损失演变以及GW和EM信号的可检测性。可以轻松地检测到来自质量损失阶段的EM信号：限制距离为〜320（M_H/10^4 m_sun）^{1/2} MPC，用于Einstein Probe。对于诸如激光干涉仪空间天线或天气之类的太空探测器的GW信号只能在局部超集群（〜33 MPC）内检测到。
During the inspiralling of a white dwarf (WD) into an intermediate-mass black hole (~ 10^{2-5} M_sun), both gravitational waves (GWs) and electromagnetic (EM) radiation are emitted. Once the eccentric orbit's pericenter radius approaches the tidal radius, the WD would be tidally stripped upon each pericenter passage. The accretion of these stripped mass would produce EM radiation. It is suspected that the recently discovered new types of transients, namely the quasi-periodic eruptions and the fast ultraluminous X-ray bursts, might originate from such systems. Modeling these flares requires a prediction of the amount of stripped mass from the WD and the details of the mass supply to the accretion disk. We run hydrodynamical simulations to study the orbital parameter dependence of the stripped mass. We find that our results match the analytical estimate that the stripped mass is proportional to z^{5/2}, where z is the excess depth by which the WD overfills its instantaneous Roche lobe at the pericenter. The corresponding fallback rate of the stripped mass is calculated, which may be useful in interpreting the individual flaring light curve in candidate EM sources. We further calculate the long-term mass-loss evolution of a WD during its inspiral and the detectability of the GW and EM signals. The EM signal from the mass-loss stage can be easily detected: the limiting distance is ~ 320(M_h/10^4 M_sun)^{1/2} Mpc for Einstein Probe. The GW signal, for the space-borne detectors such as Laser Interferometer Space Antenna or TianQin, can be detected only within the Local Supercluster (~ 33 Mpc).
