Properties of rotating neutron stars in light of binary compact object mergers

Abstract

The properties of rotating neutron stars are investigated using eight equations of state (EOSs). We also study the relations between various observables corresponding to different angular velocities for all those EOSs. All of these EoSs lead to non-rotating compact stars with maximum masses between 1.8 to 2.25 $M_{\odot }$. We calculate the moment of inertia and studied its variation with mass and the relation between central energy density and angular momentum. We compare our results with the observational findings from the most massive pulsar PSR J0740+6620 and the heaviest secondary component in the black hole - neutron star merger GW190814. It is noted that the secondary compact object of GW190814 having mass $\sim 2.6M_{\odot }$ might be explained as a rapidly rotating neutron star (NS) with frequency larger than 1000 Hz.

8 pages, 8 figures, 4 tables

References in corpus (7)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• GW190814: Gravitational Waves from the Coalescence of a 23 M${}_{\odot }$ Black Hole with a 2.6 M${}_{\odot }$ Compact Object
• Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817
• Modeling GW170817 based on numerical relativity and its implications
• New Hyperon Equations of State for Supernovae and Neutron Stars in Density-dependent Hadron Field Theory
• First 100 ms of a long-lived magnetized neutron star formed in a binary neutron star merger
• Constraining properties of rapidly rotating neutron stars using data from heavy-ion collisions