Tidal disruptions of stars by stellar-mass black holes are expected to occur
frequently in dense star clusters. Building upon previous studies that
performed hydrodynamic simulations of these encounters, we explore the
formation and long-term evolution of the thick, super-Eddington accretion disks
formed. We build a disk model that includes fallback of material from the tidal
disruption, accretion onto the black hole, and disk mass losses through winds
launched in association with the super-Eddington flow. We demonstrate that
bright transients are expected when radiation from the central engine powered
by accretion onto the black hole is reprocessed at large radii by the
optically-thick disk wind. By combining hydrodynamic simulations of these
disruption events with our disk+wind model, we compute light curves of these
wind-reprocessed transients for a wide range of stellar masses and encounter
penetration depths. We find typical peak bolometric luminosities of roughly
1041β1044erg/s (depending mostly on accretion physics parameters) and
temperatures of roughly 105β106K, suggesting peak emission in the
ultraviolet/blue bands. We predict all-sky surveys such as the Vera Rubin
Observatory and ULTRASAT will detect up to thousands of these events per year
in dense star clusters out to distances of several Gpc.Comment: 16 Pages, 13 figures, 2 tables. Accepted for publication in MNRA