The Eccentric Nature of Eccentric Tidal Disruption Events

Abstract

Upon entering the tidal sphere of a supermassive black hole, a star is ripped apart by tides and transformed into a stream of debris. The ultimate fate of that debris, and the properties of the bright flare that is produced and observed, depends on a number of parameters, including the energy of the center of mass of the original star. Here we present the results of a set of smoothed particle hydrodynamics simulations in which a $1M_{\odot }$, $\gamma =5/3$ polytrope is disrupted by a $10^6{M}_{\odot }$ supermassive black hole. Each simulation has a pericenter distance of $r_{\mathrm{p}}=r_{\mathrm{t}}$ (i.e., $\beta \equiv r_{\mathrm{t}}/r_{\mathrm{p}}=1$ with $r_{\mathrm{t}}$ the tidal radius), and we vary the eccentricity $e$ of the stellar orbit from $e=0.8$ up to $e=1.20$ and study the nature of the fallback of debris onto the black hole and the long-term fate of the unbound material. For simulations with eccentricities $e\lesssim 0.98$, the fallback curve has a distinct, three-peak structure that is induced by self-gravity. For simulations with eccentricities $e\gtrsim 1.06$, the core of the disrupted star reforms following its initial disruption. Our results have implications for, e.g., tidal disruption events produced by supermassive black hole binaries.

arXiv commentApJ Accepted

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