Tidal Stripping of a White Dwarf by an Intermediate-mass Black Hole

• Published in: The Astrophysical journal Vol. 947; no. 1; pp. 32 - 44
• Main Authors: Chen, Jin-Hong, Shen, Rong-Feng, Liu, Shang-Fei
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-04-2023; IOP Publishing
• Subjects: Accretion disks; Astronomy & Astrophysics; Astrophysics; Black holes; Eccentric orbits; Gravitational wave sources; Gravitational waves; Hydrodynamical simulations; Intermediate-mass black holes; Light curve; LISA (antenna); Radiation; Roche lobe overflow; Tidal disruption; White dwarf stars; X-ray bursts; X-ray transient sources
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/acbfb6

During the inspiralling of a white dwarf (WD) into an intermediate-mass black hole (∼10
2−5
M
⊙
), 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 this stripped mass would produce EM radiation. It is suspected that the recently discovered new types of transients, namely the quasiperiodic 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
⊙
) Mpc for the Einstein Probe. The GW signal, for space-borne detectors such as Laser Interferometer Space Antenna or TianQin, can be detected only within the Local Supercluster (∼33 Mpc).