Nucleosynthesis , light curves , explosion energies , and remnant masses are calculated for a grid of supernovae resulting from massive stars with solar metallicity and masses from 9.0 to 120 \mathrm { M } _ { \odot } .
The full evolution is followed using an adaptive reaction network of up to 2000 nuclei .
A novel aspect of the survey is the use of a one-dimensional neutrino transport model for the explosion .
This explosion model has been calibrated to give the observed energy for SN 1987A , using five standard progenitors , and for the Crab supernova using a 9.6 \mathrm { M } _ { \odot } progenitor .
As a result of using a calibrated central engine , the final kinetic energy of the supernova is variable and sensitive to the structure of each presupernova star .
Many progenitors with extended core structures do not explode , but become black holes , and the masses of exploding stars do not form a simply connected set .
The resulting nucleosynthesis agrees reasonably well with the sun provided that a reasonable contribution from Type Ia supernovae is also allowed , but with a deficiency of light s-process isotopes .
The resulting neutron star IMF has a mean gravitational mass near 1.4 \mathrm { M } _ { \odot } .
The average black hole mass is about 9 \mathrm { M } _ { \odot } if only the helium core implodes , and 14 \mathrm { M } _ { \odot } , if the entire presupernova star collapses .
Only \sim 10 % of supernovae come from stars over 20 \mathrm { M } _ { \odot } and some of these are Type Ib or Ic .
Some useful systematics of Type IIp light curves are explored .