  The evolution and explosion of metal-free stars with masses 10--100 solar
masses are followed, and their nucleosynthetic yields, light curves, and
remnant masses determined. When the supernova yields are integrated over a
Salpeter initial mass function, the resulting elemental abundance pattern is
qualitatively solar, but with marked deficiencies of odd-Z elements with 7 <= Z
<= 13. Neglecting the contribution of the neutrino wind from the neutron stars
that they make, no appreciable abundances are made for elements heavier than
germanium. The computed pattern compares favorably with what has been observed
in metal-deficient stars with [Z] ~< -3. Most of the stars end their lives as
blue supergiants and make supernovae with distinctive light curves resembling
SN 1987A, but some produce primary nitrogen by dredge up and become red
supergiants. A novel automated fitting algorithm is developed for determining
optimal combinations of explosion energy, mixing, and initial mass function in
the large model data base to agree with specified data sets. The model is
applied to the low metallicity sample of Cayrel et al. (2004) and the two
ultra-iron-poor stars HE0107-5240 and HE1327-2326. Best agreement with these
low metallicity stars is achieved with very little mixing, and none of the
metal-deficient data sets considered show the need for a high energy explosion
component. To the contrary, explosion energies somewhat less than 1.2 B seem to
be preferred in most cases. (abbreviated)
