Abstract Details

Name: Chatrik Mangat
Affiliation: Birla Institute of Technology and Science - Pilani, Hyderabad Campus, 500078
Conference ID: ASI2021_224
Title : Quasi-stationary evolution of HMNS with exotic EoS
Authors and Co-Authors : Chatrik Mangat(Birla Institute of Technology and Science - Pilani, Hyderabad Campus), Sanika Khadkikar(Birla Institute of Technology and Science - Pilani, Hyderabad Campus), Sarmistha Banik(Birla Institute of Technology and Science - Pilani, Hyderabad Campus)
Abstract Type : Poster
Abstract Category : Stars, ISM and Galaxy
Abstract : Neutron Stars (NS) are considered to be one of the most exotic objects found in this universe. The extremely dense conditions which prevail inside the neutron stars make them astrophysical laboratories of physics at extreme conditions. The recent merger event of two such neutron stars i.e. GW170817, has given an impetus to the study of the Binary Merger Remnant (BMR). A BMR is often classified as a Hyper Massive Neutron Star (HMNS). It is intuitive to discern that a rotating neutron star can support more mass than a static (non-rotating) neutron star. Building on this, a differentially rotating neutron star can support even more mass than an uniformly rotating one. Our study primarily focuses on the effect of strangeness in the evolution of an HMNS. For this, we consider both nucleonic NS, as well as NS with exotic components such as hyperons in its core. Our set of Equation of State (EoS) is compatible with the NS mass, radius and tidal deformability constraints. We assume the newly born NS to be differentially rotating initially with the maximum possible frequency. We study the same star sequence rotating uniformly at mass-shedding limit and for the static (non-rotating) case. It is theorised that a rotating NS slows down and ends up as a static star by the loss of energy and momentum via electromagnetic or gravitational radiation. Finally, we probe the quasi-stationary evolution of an HMNS between these three equilibrium sequences; along which the rest mass remains constant.