Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants

Abstract

The prediction of the equation of state of hot, dense nuclear matter is one of the most complicated and interesting problems in nuclear astrophysics. At the same time, knowledge of it is the basic ingredient for some of the most interesting studies. In the present work, we concentrate our study on the construction of the equation of state of hot, dense nuclear matter, related mainly to the interior of the neutron star. We employ a theoretical nuclear model, which includes momentum-dependent interaction among the nucleons, along with the \textit{state-of-the-art} microscopic calculations. Thermal effects are introduced in a self-consistent way, and a set of isothermal and isentropic equations of state are predicted. The predicted equations of state are used in order to acquire and to extend the knowledge of the thermal effect on both nonrotating and rapidly rotating with the Kepler frequency neutron stars. The simultaneous study of thermal and rotation effects provides useful information on some of the most important quantities, including the mass (gravitational and baryon) and radius, the Kepler frequency and Kerr parameter, the moment of inertia, etc. These quantities are directly related to studies of protoneutron stars and mainly the hot and rapidly rotating remnant of a binary neutron star merger. Data from the late observations of binary neutron star mergers and the present study may offer useful tools for their investigation and help in providing possible constraints on the equation of state of nuclear matter.

v1: 24 pages, 17 figures, 5 tables; v2: 23 pages, 18 figures, 8 tables; accepted for publication in The Astrophysical Journal

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• Probing the nuclear equation of state from the existence of a $\sim 2.6M_{\odot }$ neutron star: the GW190814 puzzle
• Twin stars as probes of the nuclear equation of state: effects of rotation through the PSR J0952-0607 pulsar and constraints via the tidal deformability from the GW170817 event
• Rapidly rotating compact stars in Rastall's gravity
• Models of binary neutron star remnants with tabulated equations of state
• Microscopic nuclear equation of state at finite temperature and stellar stability
• Thermodynamics of Hot Neutron Stars and Universal Relations
• Signatures of quark deconfinement through the r-modes of twin stars
• Unbiased interpolated neutron-star EoS at finite T for modified gravity studies
• How the HESS J1731-347 event could be explained using ${\mathbf{K}}^{-}$ condensation
• Neutron Stars and Gravitational Waves: the Key Role of Nuclear Equation of State
• Thermal effects on tidal deformability in the last orbits of an inspiraling binary neutron star system
• Hyperons and $\Delta$'s in rotating protoneutron stars: Global properties
• Determining the minimal mass of a proto-neutron star with chirally constrained nuclear equations of state
• Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?
• Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction
• Constraints on color-flavor locked quark matter in view of the HESS J1731-347 measurement
• Investigating Possible Existence of Hyper-Heavy Nuclei in Neutron Star Environment
• Rapidly Spinning Massive Pulsars as an Indicator of Quark Deconfinement
• Universal relation between dipole polarizability of finite nuclei and neutron-star compactness
• Twin stars: probe of phase transition from hadronic to quark matter
• The maximum mass and rotational kinetic energy of rapidly rotating neutron stars