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Abstract Stars approaching supermassive black holes can be tidally disrupted. Despite being expected to emit X-rays, tidal disruption events (TDEs) have been largely observed in optical bands, which is poorly understood. In this Letter, we simulate the tidal disruption of a 1 M ⊙ main-sequence star on an eccentric ( e = 0.95) orbit with a periapsis distance 1 or 5 times smaller than the tidal radius ( β = 1 or 5) using general relativistic smoothed particle hydrodynamics. We follow the simulation for up to 1 yr postdisruption. We show that accretion disks in eccentric TDEs are masked by unbound material outflowing at ∼10,000 km s −1 . Assuming electron scattering opacity, this material would be visible as a ∼100 au photosphere at ∼10 4 K, in line with observations of candidate TDEs.
Hu et al. (Tue,) studied this question.
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