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The role of compact binary mergers as the main production site of r-processelements is investigated by combining stellar abundances of Eu observed in theMilky Way, galactic chemical evolution (GCE) simulations, binary populationsynthesis models, and Advanced LIGO gravitational wave measurements. Wecompiled and reviewed seven recent GCE studies to extract the frequency ofneutron star - neutron star (NS-NS) mergers that is needed in order toreproduce the observed [Eu/Fe] vs [Fe/H] relationship. We used our simplechemical evolution code to explore the impact of different analyticaldelay-time distribution (DTD) functions for NS-NS mergers. We then combined ourmetallicity-dependent population synthesis models with our chemical evolutioncode to bring their predictions, for both NS-NS mergers and black hole -neutron star mergers, into a GCE context. Finally, we convolved our resultswith the cosmic star formation history to provide a direct comparison withcurrent and upcoming Advanced LIGO measurements. When assuming that NS-NSmergers are the exclusive r-process sites, and that the ejected r-process massper merger event is 0.01 Msun, the number of NS-NS mergers needed in GCEstudies is about 10 times larger than what is predicted by standard populationsynthesis models. These two distinct fields can only be consistent with eachother when assuming optimistic rates, massive NS-NS merger ejecta, and low Feyields for massive stars. Population synthesis models and GCE simulations arein agreement with the current upper limit (O1) established by Advanced LIGOduring their first run of observations. Upcoming measurements will provideimportant constraints on the actual local NS-NS merger rate, will provideinsights on the plausibility of the GCE requirement, and will help to definewhether or not compact binary mergers can be the dominant source of r-processelements in the Universe.

Advanced LIGO Constraints on Neutron Star Mergers and R-Process Sites