The rotating frequency and GW strain amplitude from Nuclear Models

About 96 percent mass-energy of the Universe is chargeless [1]. Thus, unlike electromagnetic radiation, it is difficult to get information from this huge part of cosmos either directly or indirectly. The only possible way to study this neutral part of the Universe is the gravitational wave (GW) radiation. The main disadvantage of the gravitational radiation is its production in laboratories. The recently measured static mass of the neutron star (NS) [2] is quite massive than the earlier measured masses. To get a larger mass, one needs a stiff EOS, which again oppose the softer EOS of kaon production [3]. To make such a model in the same footing, extra interactions are needed as it is done in G1 and G2 parametrizations [4]. In this contribution, we have taken 20 different EOS’s from both nonrelativistic Skyrme and relativistic mean field (RMF) formalisms and calculate the gravitational wave strain amplitude (h0) of rotating neutron star (RNS).