Studying VLOCV twin compact stars with binary mergers

Abstract

GW170817 has provided valuable constraints on the equations of state of merging binary neutron stars, which can be considered as the most probable candidate for the source of gravitational waves. On the other hand, these natural laboratories of extreme temperature and density may lead to the estimation of some exotic matter like {deconfined quark matter in their cores}. In this paper, we investigate the neutron star matter equation of state (EoS) with the lowest order constrained variational (LOCV) method considering the excluded volume effect (VLOCV) for nucleons {to} compute the tidal deformability of binary neutron star mergers (BNSMs). Within this approach, the size of nucleons makes the EoS {so} stiff that requires a phase transition in order to avoid causality violation. Therefore, this phase transition {may lead} to the appearance of the third family of compact stars {including} ``twin star'' configurations. {Our EoS models are confronted with observations from GW170817, GW190814, GW190425, and also NICER. We find out that regarding all these constraints, the EoS models having the {transition} pressure$\approx$30-100 MeV/fm${}^3$ and the energy density discontinuity $\Delta \epsilon$$\lesssim$300 MeV/fm${}^3$ are preferable.

arXiv comment24 pages, 7 figures

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• Speed of Sound in Hybrid Stars and the Role of Bag Pressure in the Emergence of Special Points on M-R Variation of Hybrid Stars
• XTE J1814-338: A potential hybrid star candidate
• A Detailed Analysis of the Special Points on $M-R$ Solutions of Hybrid (Twin) Stars
• Speed of sound bounds and first-order phase transitions in compact stars
• Signatures of quark deconfinement through the r-modes of twin stars
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• Properties of the Object HESS J1731-347 as a Twin Compact Star
• Binary neutron star mergers within kaon condensation: GW170817
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