  A rudimentary calculation is employed to evaluate the possible effects of
beta- decays of excited-state nuclei on the astrophysical r-process.
Single-particle levels calculated with the FRDM are adapted to the calculation
of beta-decay rates of these excited-state nuclei. Quantum numbers are
determined based on proximity to Nilson model levels. The resulting rates are
used in an r-process network calculation in which a supernova hot-bubble model
is coupled to an extensive network calculation including all nuclei between the
valley of stability and the neutron drip line and with masses A<284. Beta-decay
rates are included as functional forms of the environmental temperature. While
the decay rate model used is simple and phenomenological, it is consistent
across all 3700 nuclei involved in the r-process network calculation. This
represents an approximate first estimate to gauge the possible effects of
excited-state beta-decays on r-process freeze-out abundances.
