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In this paper, we discuss the damping of density oscillations in densenuclear matter in the temperature range relevant to neutron star mergers. Thisdamping is due to bulk viscosity arising from the weak interaction ``Urca''processes of neutron decay and electron capture. The nuclear matter is modelledin the relativistic density functional approach. The bulk viscosity reaches aresonant maximum close to the neutrino trapping temperature, then drops rapidlyas temperature rises into the range where neutrinos are trapped in neutronstars. We investigate the bulk viscous dissipation timescales in a post-mergerobject and identify regimes where these timescales are as short as thecharacteristic timescale $\sim$10 ms, and, therefore, might affect theevolution of the post-merger object. Our analysis indicates that bulk viscousdamping would be important at not too high temperatures of the order of a fewMeV and densities up to a few times saturation density.

Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers