  Stars approaching supermassive black holes can be tidally disrupted. Despite
being expected to emit X-rays, TDEs have been largely observed in optical
bands, which is poorly understood. In this Letter, we simulate the tidal
disruption of a $1~M_\odot$ main sequence star on an eccentric ($e=0.95$) orbit
with a periapsis distance one or five times smaller than the tidal radius
($\beta = 1$ or $5$) using general relativistic smoothed particle
hydrodynamics. We follow the simulation for up to a year post-disruption. We
show that accretion disks in eccentric TDEs are masked by unbound material
outflowing at $\sim10,000~$km/s. Assuming electron scattering opacity, this
material would be visible as a $\sim100~$au photosphere at $\sim10^4~$K, in
line with observations of candidate TDEs.
