  A star completely destroyed in a tidal disruption event (TDE) ignites a
luminous flare that is powered by the fallback of tidally stripped debris to a
supermassive black hole (SMBH) of mass $M_{\bullet}$. We analyze two estimates
for the peak fallback rate in a TDE, one being the "frozen-in" model, which
predicts 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 postulates
that the star is completely destroyed when tides dominate the maximum stellar
self-gravity, predicts that $t_{\rm peak}$ is very weakly dependent on stellar
type, with $t_{\rm peak} = \left(23.2\pm4.0\textrm{
days}\right)\left(M_{\bullet}/10^6M_{\odot}\right)^{1/2}$ for $0.2\le
M_{\star}/M_{\odot} \le 5$, while $t_{\rm peak} = \left(29.8\pm3.6\textrm{
days}\right)\left(M_{\bullet}/10^6M_{\odot}\right)^{1/2}$ for a Kroupa initial
mass function truncated at $1.5 M_{\odot}$. This second estimate also agrees
closely with hydrodynamical simulations, while the frozen-in model is
discrepant by orders of magnitude. We conclude that (1) the time to peak
luminosity 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-Eddington
TDEs are powered by the complete disruption of massive stars, which -- if
responsible for producing jetted TDEs -- would explain the rarity of jetted
TDEs and their preference for young and star-forming host galaxies.
