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The exact evolution of elements in the universe, from primordial to heavierelements produced via the r-process, is still under scrutiny. The supernovadeaths of the very first stars led to the enrichment of their localenvironments, and can leave behind neutron stars (NS) as remnants. Theseremnants can end up in binary systems with other NSs, and eventually merge,allowing for the r-process to occur. We study the scenario where a single NSmerger (NSM) enriches a halo early in its evolution to understand the impact onthe second generation of stars and their metal abundances. We perform a suiteof high resolution cosmological zoom-in simulations using Enzo where we haveimplemented a new NSM model varying the explosion energy and the delay time. Ingeneral, a NSM leads to significant r-process enhancement in the secondgeneration of stars in a galaxy with a stellar mass of $\sim 10^5\mathrm{M}_{\odot}$ at redshift 10. A high explosion energy leads to a Pop IImass fraction of 72% being highly enhanced with r-process elements, while alower explosion energy leads to 80% being enhanced, but only 14% being highlyenhanced. When the NSM has a short delay time of 10 Myr, only 5% of the massfraction of Pop II stars is highly enhanced, while 64% is highly enhanced forthe longest delay time of 100 Myr. This work represents a stepping stonetowards understanding how NSMs impact their environments and metal abundancesof descendant generations of stars.

Neutron Star Mergers and their Impact on Second Generation Star Formation in the Early Universe