Binary neutron star mergers within kaon condensation: GW170817

Abstract

The equation of state (EoS) of neutron star (NS) matter is investigated considering kaon condensation. Moreover, the tidal parameters related to the components of binary neutron star mergers are determined and compared to the constraints of GW170817 imposed on these quantities. In this study, we employ the lowest-order constrained variational (LOCV) approach and utilize {AV6${}^{\prime }$, AV8${}^{\prime }$, and AV18 potentials} accompanied by the three nucleon interaction (TNI) {in order to consider the nucleon-nucleon interaction}. It is known that the existence of kaons in the core of NSs softens the EoS {and thus} lowers the value of maximum mass which is expected to be greater than 2 M${}_{\odot }$. Our results demonstrate that considering kaon condensation with a strangeness value, a${}_3$m${}_s$=-134 MeV satisfies the maximum mass constraint except for AV8${}^{\prime }$+TNI potential. However, the calculation of dimensionless tidal deformability shows that with the decrease of strangeness value, the neutron star gets less deformed.

arXiv comment20 pages, 8 figures

References in corpus (22)

• 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
• GW190425: Observation of a Compact Binary Coalescence with Total Mass $\sim 3.4M_{\odot }$
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• Nonequilibrium Weak Processes in Kaon Condensation II - Kinetics of condensation ---
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Cited by in corpus (1)

• How the HESS J1731-347 event could be explained using ${\mathbf{K}}^{-}$ condensation