We investigate the significance of isomers on a kilonova associated with neutron star mergers (NSMs) for the first time. We calculate the evolution of abundances and energy generation rates ($\dot{ \epsilon}_{ \rm nuc}$) of ejecta from NSMs, taking into account $\beta^-$ decay through isomers. We find that for ejecta with electron fraction ($Y_e$) of $0.2-0.3$, $\dot{ \epsilon}_{ \rm nuc}$ is appreciably changed from those without isomers, due to the large change in timing of $\beta^-$ decay through the isomeric states of ${ }^{ 123, 125, 127} \rm Sn$ and ${ }^{ 128} \rm Sb$. In particular, the effects of the isomers on $\dot{ \epsilon}_{ \rm nuc}$ are prominent for ejecta of $Y_e \sim 0.25$, which could emit a fraction of an early, blue component of a kilonova observed in GW170817. When the excitation from a ground state to its isomeric state is important, the isomers of ${ }^{ 129} \rm Sb$ and ${ }^{ 129, 131} \rm Te$ also cause additional and appreciable change in $\dot{ \epsilon}_{ \rm nuc}$. Furthermore, we demonstrate that larger amounts of lanthanide-free ejecta result in a better fit of an observed light curve of the kilonova in GW170817 if the isomers are taken into account.
Categories: astro-ph.HE nucl-th