  Nucleosynthesis beyond Fe poses additional challenges not encountered when
studying astrophysical processes involving light nuclei. Astrophysical sites
and conditions are not well known for some of the processes involved. On the
nuclear physics side, different approaches are required, both in theory and
experiment. The main differences and most important considerations are
presented for a selection of nucleosynthesis processes and reactions,
specifically the $s$-, $r$-, $\gamma$-, and $\nu p$-processes. Among the
discussed issues are uncertainties in sites and production conditions, the
difference between laboratory and stellar rates, reaction mechanisms, important
transitions, thermal population of excited states, and uncertainty estimates
for stellar rates. The utility and limitations of indirect experimental
approaches are also addressed. The presentation should not be viewed as
confining the discussed problems to the specific processes. The intention is to
generally introduce the concepts and possible pitfalls along with some
examples. Similar problems may apply to further astrophysical processes
involving nuclei from the Fe region upward and/or at high plasma temperatures.
The framework and strategies presented here are intended to aid the conception
of future experimental and theoretical approaches.
