Equation of state effects in the core collapse of a 
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Schneider, A.; Roberts, Luke F.; Ott, Christian D.; O’Connor, Evan

doi:10.1103/physrevc.100.055802

Cited by 83 publications

(85 citation statements)

References 111 publications

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“…T C being the critical temperature. One of the basic and fundamental quantity of the NM is incompressibility, also known as the isoscalar incompressibility or compression modulus (K ) [8]. K directly influences the curvature of the equation of state and gives adequate information about the nature of the equation of state.…”

Section: Theoretical Formalismmentioning

confidence: 99%

“…Since it is believed that the matter evolved during the core-collapse phenomenon is unable to attain β−equilibrium condition for few seconds [6], due to the promptness of the CCSN explosion, so, usually the EoS for a dense matter with either same amount of protons and neutrons or a proton fraction of ∼ 0.2 is taken into account to cipher the dynamics of collapse event [7]. Many other important aspects of core-collapse events like how many protons are converted into neutrons, quenching rate, the mass-radius profile of newly born neutron star and its composition are determined by the EoS [8].…”

Section: Introductionmentioning

confidence: 99%

“…The isovector skewness parameter (Q sym ) is the most ambiguous quantity, due to the large fluctuations in its value obtained from different models. Recent studies show that Q sym is related to the incompressibility [22] of the system and also suggest an important role of Q sym in the cooling of newly born proto-neutron star [8]. We study in detail the effects of temperature on all these nuclear parameters and the correlations among them using the most familiar NL3, IU-FSU and recently developed G3 parameter sets.…”

Section: Introductionmentioning

confidence: 99%

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Warm dense matter and cooling of supernovae remnants

et al. 2020

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We study the thermal effects on the nuclear matter (NM) properties such as binding energy, incompressibility, free symmetry energy and its coefficients using NL3, G3 and IU-FSU parameter sets of relativistic mean-field models. These models being consistent with the properties of cold NM, have also been used to study the effect of temperature by incorporating the Fermi function. The critical temperature for the liquid-gas phase transition in the symmetric NM is found to be 14.60, 15.37 and 14.50 MeV for NL3, G3 and IU-FSU parameter sets respectively, which is in excellent agreement with previous theoretical and experimental studies. We inspect that the properties related to second differential coefficient of the binding energy and free symmetry energy at saturation density ( i.e. $$K_{0}(n,T)$$K0(n,T) and $$Q_{sym,0}$$Qsym,0 ) exhibit the contrary effects for NL3 and G3 parameters as the temperature increases. We find that the prediction of saturated curvature parameter ( $$K_{sym,0}$$Ksym,0 ) for G3 equation of state at finite temperature favour the combined analysis of $$K_{sym,0}$$Ksym,0 for the existence of massive pulsars, gravitational waves from GW170817 and NICER observations of PSR J0030+0451. Further, we investigate the cooling mechanism of newly born stars through neutrino emissivity controlled by direct Urca process and instate some interesting remarks about neutrino emissivity. We also deliberate the effect of temperature on the M-R profile of Proto-Neutron star.

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Section: Theoretical Formalismmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Warm dense matter and cooling of supernovae remnants

et al. 2020

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“…Recent fits of the APR calculations to the traditional Skyrme energy-density functional (EDF) can be found in Refs. [90,91]. The latter also details the calculation of a complete tabular EoS based on the original APR parametric form.…”

Section: Nucleonic Eossmentioning

confidence: 99%

Treating quarks within neutron stars

et al. 2019

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Neutron star interiors provide the opportunity to probe properties of cold dense matter in the QCD phase diagram. Utilizing models of dense matter in accord with nuclear systematics at nuclear densities, we investigate the compatibility of deconfined quark cores with current observational constraints on the maximum mass and tidal deformability of neutron stars. We explore various methods of implementing the hadron-to-quark phase transition, specifically, first-order transitions with sharp (Maxwell construction) and soft (Gibbs construction) interfaces, and smooth crossover transitions. We find that within the models we apply, hadronic matter has to be stiff for a first-order phase transition and soft for a crossover transition. In both scenarios and for the equations of state we employed, quarks appear at the center of pre-merger neutron stars in the mass range ≈ 1.0 − 1.6 M , with a squared speed of sound c 2 QM 0.4 characteristic of strong repulsive interactions required to support the recently discovered neutron star masses ≥ 2 M . We also identify equations of state and phase transition scenarios that are consistent with the bounds placed on tidal deformations of neutron stars in the recent binary merger event GW170817. We emphasize that distinguishing hybrid stars with quark cores from normal hadronic stars is very difficult from the knowledge of masses and radii alone, unless drastic sharp transitions induce distinctive disconnected hybrid branches in the mass-radius relation.

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“…In addition, microscopic approaches based on realistic nuclear forces have been also applied to construct the EOS tables for astrophysical simulations (Togashi et al 2017;Furusawa et al 2017b). In Schneider et al (2019), the authors developed the EOS tables based on the Skyrme-type parameterization of the nuclear force, where the parameters were tuned to reproduce the Akmal, Pandharipande, and Ravenhall (APR) EOS.…”

Section: Introductionmentioning

confidence: 99%

Effects of Symmetry Energy on the Equation of State for Simulations of Core-collapse Supernovae and Neutron-star Mergers

Shen

et al. 2020

ApJ

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We construct a new equation of state (EOS) for numerical simulations of core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with a small symmetry energy slope L, which is compatible with both experimental nuclear data and recent observations of neutron stars. The new EOS table (EOS4) based on the extended TM1 (TM1e) model with L = 40 MeV is designed in the same tabular form and compared with the commonly used Shen EOS (EOS2) based on the original TM1 model with L = 110.8 MeV. This is convenient and useful for performing numerical simulations and examining the influences of symmetry energy and its density dependence on astrophysical phenomena. In comparison with the TM1 model used in EOS2, the TM1e model provides a similar maximum neutron-star mass but smaller radius and tidal deformability for a 1.4M ⊙ neutron star, which is more consistent with current constraints. By comparing the phase diagram and thermodynamic quantities between EOS4 and EOS2, it is found that the TM1e model predicts relatively larger region of nonuniform matter and softer EOS for neutron-rich matter. Significant differences between EOS4 and EOS2 are observed in the case with low proton fraction, while the properties of symmetric matter remain unchanged.

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Equation of state effects in the core collapse of a 20−M⊙ star

Cited by 83 publications

References 111 publications

Warm dense matter and cooling of supernovae remnants

Warm dense matter and cooling of supernovae remnants

Treating quarks within neutron stars

Effects of Symmetry Energy on the Equation of State for Simulations of Core-collapse Supernovae and Neutron-star Mergers

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