  About half of the elements beyond iron are synthesized in stars by
rapid-neutron capture process (r-process). The stellar environment provides
very high neutron flux in a short time ($\sim$ seconds) which is conducive for
the creation of progressively neutron-rich nuclei till the waiting point is
reached after which no further neutron capture reactions proceed. At this point
such extremely neutron-rich nuclei become stable via $\beta^-$ decay. A
detailed understanding of the r-process remains illusive. In the present work,
we explore the radiative neutron-capture (n,$\gamma$) cross sections and
reaction rates around the r-process peak near mass number eighty. The inherent
uncertainties remain large in some cases, particularly in case of neutron-rich
nuclei. When the low-energy enhancement exists, it results in significant
increase in the reaction rate for neutron-capture.
