Detection of a gravitational wave (GW) signal in 2017 (GW170817) by the LIGO-Virgo collaboration coming from a binary neutron star (BNS) merger, complemented by the detection of its electromagnetic counterpart paved the way for a new age of multi-messenger astronomy. In combination with other ground-breaking observations in the recent past, viz., observation of the two solar mass neutron stars (NS) with the Shapiro delay technique, or the combined mass-radius measurement of NS with NASA's NICER X-ray telescope, nuclear physics input in the modeling of compact stars became a real necessity now. Moreover, we are on the brink of having next-generation ground-based interferometers like the Einstein Telescope (ET) or Cosmic Explorer (CE), where the number of GW detections will increase in manifolds due to their highly enhanced sensitivity. This includes the detection of signals from post-merger oscillations of hypermassive NSs or proto-neutron stars at the brink of core-collapse supernovae. Synergy in the modeling of these complex astrophysical phenomena taking into account microphysical inputs of the structure of dense nuclear matter is thus one of the needs of the hour. Moreover, in the neutron star environment, there are answers to many crucial questions regarding dense matter, one of the most important being the existence (or not) of hadronic to the quark phase transition in the inner core of massive neutron stars. In the present talk, I will demonstrate a few recent results I have obtained to address some of these questions. I will also outline my future plan which can help further to build a synergy of gravitational wave astronomy and microscopic nuclear physics.
