  We survey the properties of stars destroyed in TDEs as a function of BH mass,
stellar mass and evolutionary state, star formation history and redshift. For
Mbh<10^7Msun, the typical TDE is due to a M*~0.3Msun M-dwarf, although the mass
function is relatively flat for $M*<Msun. The contribution from older main
sequence stars and sub-giants is small but not negligible. From
Mbh~10^7.5-10^8.5Msun, the balance rapidly shifts to higher mass stars and a
larger contribution from evolved stars, and is ultimately dominated by evolved
stars at higher BH masses. The star formation history has little effect until
the rates are dominated by evolved stars. TDE rates should decline very rapidly
towards higher redshifts. The volumetric rate of TDEs is very high because the
BH mass function diverges for low masses. However, any emission mechanism which
is largely Eddington-limited for low BH masses suppresses this divergence in
any observed sample and leads to TDE samples dominated by Mbh~10^6.0-10^7.5Msun
BHs with roughly Eddington peak accretion rates. The typical fall back time is
relatively long, with 16% having Tfb<10^(-1) years (37 days), and 84% having
longer time scales. Many residual rate discrepancies can be explained if
surveys are biased against TDEs with these longer Tfb, which seems very
plausible if Tfb has any relation to the transient rise time. For almost any BH
mass function, systematic searches for fainter, faster time scale TDEs in
smaller galaxies, and longer time scale TDEs in more massive galaxies are
likely to be rewarded.
