Hot quark matter and merger remnants

TL;DR

This study models hot quark matter in neutron star merger remnants using a novel temperature-inclusive DDQM approach, revealing how entropy and temperature influence remnant structure, particle distribution, and compliance with observed neutron star masses.

Contribution

Introduces a temperature-dependent DDQM model for simulating hot quark matter in neutron star mergers, incorporating lattice QCD insights for the first time.

Findings

Remnant mass and size increase with entropy.

Neutrino abundance rises with entropy.

Strange-quark star remnants meet 2 solar mass constraint.

Abstract

This work investigates hot quark matter under the thermodynamic conditions characteristic of a binary neutron star (BNS) merger remnants. We used the density-dependent quark mass model (DDQM) to access the microscopic nuclear equation of state (EoS) in a series of snapshots. The strange quark matter (SQM) is studied at finite temperature and entropy, in the presence of electrons and muons and their corresponding neutrinos to simulate the BNS merger conditions. For the first time, we introduced temperature into the DDQM model using a lattice QCD-motivated approach to construct both isentropic and isothermal EoSs. We observe that as the entropy of the SQM increases, the merger remnant becomes more massive and increases in size, whereas the neutrino abundance also increases. In the fixed-temperature case, on the other hand, we observe that the entropy spreads from the surface towards the center of the remnant. We determine the particle distribution in the core of the remnants, the structure of the remnant, the temperature profile, sound velocity, and the polytropic index, and discuss their effects. The strange-quark star (SQS) remnants satisfy the $2\,{\rm M_\odot}$ mass constraint associated with neutron stars (NS).