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A star completely destroyed in a tidal disruption event (TDE) ignites aluminous flare that is powered by the fallback of tidally stripped debris to asupermassive black hole (SMBH) of mass $M_{\bullet}$. We analyze two estimatesfor the peak fallback rate in a TDE, one being the "frozen-in" model, whichpredicts a strong dependence of the time to peak fallback rate, $t_{\rm peak}$,on both stellar mass and age, with $15\textrm{ days} \lesssim t_{\rm peak}\lesssim 10$ yr for main sequence stars with masses $0.2\le M_{\star}/M_{\odot}\le 5$ and $M_{\bullet} = 10^6M_{\odot}$. The second estimate, which postulatesthat the star is completely destroyed when tides dominate the maximum stellarself-gravity, predicts that $t_{\rm peak}$ is very weakly dependent on stellartype, with $t_{\rm peak} = \left(23.2\pm4.0\textrm{days}\right)\left(M_{\bullet}/10^6M_{\odot}\right)^{1/2}$ for $0.2\leM_{\star}/M_{\odot} \le 5$, while $t_{\rm peak} = \left(29.8\pm3.6\textrm{days}\right)\left(M_{\bullet}/10^6M_{\odot}\right)^{1/2}$ for a Kroupa initialmass function truncated at $1.5 M_{\odot}$. This second estimate also agreesclosely with hydrodynamical simulations, while the frozen-in model isdiscrepant by orders of magnitude. We conclude that (1) the time to peakluminosity in complete TDEs is almost exclusively determined by SMBH mass, and(2) massive-star TDEs power the largest accretion luminosities. Consequently,(a) decades-long extra-galactic outbursts cannot be powered by complete TDEs,including massive-star disruptions, and (b) the most highly super-EddingtonTDEs are powered by the complete disruption of massive stars, which -- ifresponsible for producing jetted TDEs -- would explain the rarity of jettedTDEs and their preference for young and star-forming host galaxies.

The Peak of the Fallback Rate from Tidal Disruption Events: Dependence on Stellar Type