  We performed a Penning trap mass measurement of $^{61}{\rm Zn}$ at the
National Superconducting Cyclotron Laboratory and NuShellX calculations of the
$^{61}{\rm Zn}$ and $^{62}{\rm Ga}$ structure using the GXPF1A Hamiltonian to
obtain improved estimates of the $^{61}{\rm Zn}(p,\gamma)^{62}{\rm Ga}$ and
$^{60}{\rm Cu}(p,\gamma)^{61}{\rm Zn}$ reaction rates. Surveying astrophysical
conditions for type-I X-ray bursts with the code MESA, implementing our
improved reaction rates, and taking into account updated nuclear masses for
$^{61}{\rm V}$ and $^{61}{\rm Cr}$ from the recent literature, we refine the
neutrino luminosity from the important mass number $A=61$ urca cooling source
in accreted neutron star crusts. This improves our understanding of the thermal
barrier between deep heating in the crust and the shallow depths where extra
heat is needed to explain X-ray superbursts, as well as the expected signature
of crust urca neutrino emission in light curves of cooling transients.
