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A tidal disruption event (TDE) takes place when a star passes near enough toa massive black hole to be disrupted. About half the star's matter is givenelliptical trajectories with large apocenter distances, the other half isunbound. To "circularize", i.e., to form an accretion flow, the bound mattermust lose a significant amount of energy, with the actual amount depending onthe characteristic scale of the flow measured in units of the black hole'sgravitational radius ($\sim 10^{51} (R/1000R_g)^{-1}$~erg). Recent numericalsimulations \citep{Shiokawa+2015} have revealed that the circularization scaleis close to the scale of the most-bound initial orbits, $\sim 10^3M_{BH,6.5}^{-2/3} R_g \sim 10^{15} M_{BH,6.5}^{1/3}$~cm from the black hole,and the corresponding circularization energy dissipation rate is $\sim 10^{44}M_{BH,6.5}^{-1/6}$~erg/s. We suggest that the energy liberated duringcircularization, rather then energy liberated by accretion onto the black hole,powers the observed optical TDE candidates. The observed rise times,luminosities, temperatures, emission radii, and line widths seen in these TDEs\citep[e.g.][]{Arcavi+2014} are all more readily explained in terms of heatingassociated with circularization than in terms of accretion.

"Circularization" vs. Accretion -- What Powers Tidal Disruption Events?