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The disruption of a star by a supermassive black hole generates a suddenbright flare. Previous studies have focused on the disruption by single blackholes, for which the fallback rate decays as~$\propto t^{-5/3}$. In this paper,we generalise the study to the case of a supermassive black hole binary(SMBHB), using both analytical estimates and hydrodynamical simulations,looking for specific observable signatures. The range of binary separation forwhich it is possible to distinguish between the disruption created by a singleor a binary black hole concerns typically separations of order a fewmilliparsecs for a primary of mass $\sim 10^6M_{\odot}$. When the fallback rateis affected by the secondary, it undergoes two types interruptions, dependingon the initial inclination $\theta$ of the orbit of the star relative to theplane of the SMBHB. For $\theta \lesssim 70^\circ$, periodic sharpinterruptions occur and the time of first interruption depends on the distanceof the secondary black hole with the debris. If $\theta \gtrsim 70^\circ$, afirst smooth interruption occurs, but not always followed by a further recoveryof the fallback rate. This implies that most of the TDEs around a SMBHB willundergo periodic sharp interruptions of their lightcurve.

Tidal disruption of stars in a supermassive black hole binary system: the influence of orbital properties on fallback and accretion rates