Abstract A repeating partial tidal disruption event (rpTDE) is typically modeled as a star on a bound orbit that is partially disrupted by a massive black hole (MBH) at each pericenter passage. For disruption to occur, the pericenter distance must be close to or within the characteristic tidal radius, such that the tidal field overcomes the star’s binding force and triggers mass loss. However, a binary with a pericenter distance several times the tidal radius can build up its tidal perturbation over multiple orbits via a diffusive process, eventually triggering a nonlinear instability that ejects mass and powers an eruption. This leads to repeated, stochastic disruptions. In this Letter, we propose that such a mechanism can produce a subclass of rpTDEs with large variations in recurrence time (e.g., J0456–20), which we dub “diffusive-tide rpTDEs.” We show that diffusive tidal growth can occur for a white dwarf or main-sequence star orbiting a MBH when the pericenter distance is a few times the tidal radius, provided that the orbital period is shorter than the tidal energy dissipation timescale. These diffusive-tide rpTDEs may account for a significant fraction of the rpTDE population.
Lau et al. (Fri,) studied this question.
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