Abstract
White dwarf stars that enter the tidal radius of black holes with masses \(\lesssim 10^{5}~\text{M}_{\odot }\) are doomed to be ripped apart by tidal forces. Black holes in this mass range between stellar black holes and supermassive black holes have not been conclusively identified so the detection of a tidal disruption of a white dwarf would provide clear evidence for the existence of intermediate-mass black holes. In this review, we present a theoretical and observational overview of the transient events that result from the tidal disruptions of white dwarfs by intermediate-mass black holes. This includes discussion of the latest simulations and predicted properties, the results of observational searches, as well as a summary of the potential for gravitational wave emission to be detected with upcoming missions.
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Notes
The mass fraction of H was taken to be \(10^{-5}\) and other elements were assumed to have their Solar mass fractions.
Although the process of circularisation of the gas stream in white dwarf disruptions is affected by General Relativistic effects in contrast to many main sequence TDEs; see the contribution from Bonnerot et al. in this Volume on the formation of the accretion flow after disruption.
The integral of the Schechter function can be expressed in terms of incomplete \(\Gamma \) functions, \(\Gamma (p,a)=\int _{a}^{\infty }x^{p-1}e^{-x}\, dx\).
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The Tidal Disruption of Stars by Massive Black Holes
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Maguire, K., Eracleous, M., Jonker, P.G. et al. Tidal Disruptions of White Dwarfs: Theoretical Models and Observational Prospects. Space Sci Rev 216, 39 (2020). https://doi.org/10.1007/s11214-020-00661-2
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DOI: https://doi.org/10.1007/s11214-020-00661-2