  We estimate lepton capture and emission rates, as well as neutrino energy
loss rates, for nuclei in the mass range A=65-80. These rates are calculated on
a temperature/density grid appropriate for a wide range of astrophysical
applications including simulations of late time stellar evolution and x-ray
bursts. The basic inputs in our single particle and empirically inspired model
are i) experimentally measured level and weak decay information, ii) estimates
of matrix elements for allowed experimentally-unmeasured transitions based on
the systematics of experimentally observed allowed transitions, and iii)
estimates of the centroids of the GT resonances motivated by shell model
calculations in the fp shell as well as by (n,p) and (p,n) experiments.
Transitions involving Fermi resonances (isobaric analog states) are also
included and dominate the rates for many interesting proton rich nuclei for
which an experimentally-determined ground state lifetime is unavailable. To
compare our results with more detailed shell model based calculations we also
calculate weak rates for nuclei in the mass range A=60-65 for which Langanke
and Martinez-Pinedo have provided rates. The typical deviation in the electron
capture and B- decay rates for these ~30 nuclei is less than a factor of two or
three for a wide range of temperature and density appropriate for pre-supernova
stellar evolution. We also discuss some subtleties associated with the
partition functions used in calculations of stellar weak rates and show that
the proper treatment of the partition functions is essential for estimating
high temperature beta decay rates. Partition functions based on un-converged
Lanczos calculations can result in estimates of high temperature beta decay
rates that are systematically low.
