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Liu and collaborators recently proposed an elliptical accretion disk modelfor tidal disruption events (TDEs). They showed that the accretion disks ofoptical/UV TDEs are large and highly eccentric and suggested that the broadoptical emission lines with complex and diverse profiles originate in the cooleccentric accretion disk of random inclination and orientation. In this paper,we calculate the radiation efficiency of the elliptical accretion disk andinvestigate the implications for the observations of TDEs. We compileobservational data for the peak bolometric luminosity and total radiationenergy after peak brightness of 18 TDE sources and compare these data to thepredictions from the elliptical accretion disk model. Our results show that theobservations are consistent with the theoretical predictions and that themajority of the orbital energy of the stellar debris is advected into the blackhole (BH) without being converted into radiation. Furthermore, we derive themasses of the disrupted stars and the masses of the BHs of the TDEs. The BHmasses obtained in this paper are also consistent with those calculated withthe $M_{\rm BH} - \sigma_*$ relation. Our results provide an effective methodfor measuring the masses of BHs in large numbers of TDEs to be discovered inongoing and next-generation sky surveys, regardless of whether the BHs arelocated at the centers of galactic nuclei or wander in disks and halos.

Measuring black hole masses from tidal disruption events and testing the $M_{\rm BH}-\sigma_*$ relation