The multimessenger detection of GW170817 event has brought us first direct evidence that binary neutron star mergers are one of the major sites producing elements heavier than iron. This represents a first step towards obtaining the full understanding of heavy element production history of the universe. Concordant efforts involving further progress from different fields, including astrophysical source modeling, (chemical) evolution of galaxies, microphysics (nuclear physics and particle physics) inputs, and various astronomical observations are needed to paint a full picture. In this talk, I will first give an overview of the current status and mention issues going forward. I will then discuss our recent contributions to a few different topics including the role of nuclear physics inputs and neutrino flavor oscillations, some aspects of the galactic chemical evolution of r-process elements, and our on-going efforts.