Hot neutron stars with microscopic equations of state

Lu, Jia-Jing; Li, Zeng-Hua; Burgio, G. F.; Figura, A.; Schulze, H.-J.

doi:10.1103/physrevc.100.054335

Cited by 45 publications

(41 citation statements)

References 98 publications

(80 reference statements)

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“…The free energy density decreases with temperature. Consistent with the results of [13,19,31,15,14,25], I find that the decrease is more prominent at low baryon densities since the thermal effects on nuclear matter are more dominant at this density regime. With the increase of baryon density, the effect of temperature gradually reduces and therefore the free energy isotherms almost converge at high density.…”

Section: Symmetric Nuclear Matter At Low Density and Finite Temperaturesupporting

confidence: 90%

“…In this work I have therefore treated matter as asymmetric and re-computed some of the properties of such matter like the EoS and the speed of sound. As mentioned earlier that nuclear matter at high density is highly applicable to account for the composition of PNSs and consequently their structural properties [3,64,49,65,66,9,31,67,4,13,15,68,69,18,23,5,19]. In the present work I considered β equilibrated matter at finite temperature and for the neutrino untrapped scenario [3,69,9,13], I investigated the role of temperature to determine the static properties of PNSs like gravitational and baryonic mass, radius and the surface redshift.…”

Section: Introductionmentioning

confidence: 99%

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Nuclear matter at finite temperature and static properties of proto-neutron star

Sen¹

2020

J. Phys. G: Nucl. Part. Phys.

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With the effective chiral model, the finite temperature properties of nuclear matter have been studied at different temperatures. For symmetric nuclear matter, I particularly focused on the possibility of liquid-gas phase transition at low temperature and density. The critical temperature obtained in this context, is consistent with the experimental and empirical findings. The free energy and entropy variation are also studied for different values of temperature. A few asymmetric nuclear matter properties like the equation of state and the speed of sound with respect to temperature are also examined. The work is also extended to obtain the equation of state β stable nuclear matter at finite temperature. For the neutrino free case, the various static proto-neutron star properties are computed for a wide range of temperature, relevant to proto-neutron stars. For all the values of temperature, the obtained estimates of maximum gravitational mass are found to be in good agreement with the observational constraints specified from massive pulsars like PSR J0348+0432 and PSR J0740+6620. The results of surface redshift for all the temperature also satisfy the maximum surface redshift constraints from EXO 07482-676, 1E 1207.4-5209 and RX J0720.4-3125.

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Section: Symmetric Nuclear Matter At Low Density and Finite Temperaturesupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Nuclear matter at finite temperature and static properties of proto-neutron star

Sen¹

2020

J. Phys. G: Nucl. Part. Phys.

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“…EoSs at finite temperature constructed within the Brueckner-Hartree-Fock approach and the properties of hot β-stable nuclear matter were studied in a series of papers [37][38][39][40][41][42][43][44][45].…”

Section: Introductionmentioning

confidence: 99%

Neutron Stars and Gravitational Waves: The Key Role of Nuclear Equation of State

Koliogiannis¹,

Kanakis-Pegios²,

Moustakidis³

2021

Foundations

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Neutron stars are the densest known objects in the universe and an ideal laboratory for the strange physics of super-condensed matter. Theoretical studies in connection with recent observational data of isolated neutron stars, as well as binary neutron stars systems, offer an excellent opportunity to provide robust solutions on the dense nuclear problem. In the present work, we review recent studies concerning the applications of various theoretical nuclear models on a few recent observations of binary neutron stars or neutron-star–black-hole systems. In particular, using a simple and well-established model, we parametrize the stiffness of the equation of state with the help of the speed of sound. Moreover, in comparison to the recent observations of two events by LIGO/VIRGO collaboration, GW170817 and GW190425, we suggest possible robust constraints. We also concentrate our theoretical study on the resent observation of a compact object with mass ∼2.59−0.09+0.08M⊙ (GW190814 event), as a component of a system where the main companion was a black hole with mass ∼23M⊙. There is scientific debate concerning the identification of the low mass component, as it falls into the neutron-star–black-hole mass gap. This is an important issue since understanding the nature of GW190814 event will offer rich information concerning the upper limit of the speed of sound in dense matter and the possible phase transition into other degrees of freedom. We systematically study the tidal deformability of a possible high-mass candidate existing as an individual star or as a component in a binary neutron star system. Finally, we provide some applications of equations of state of hot, dense nuclear matter in hot neutron stars (nonrotating and rapidly rotating with the Kepler frequency neutron stars), protoneutron stars, and binary neutron star merger remnants.

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“…While a large number of phenomenological and microscopic EOSs is available for investigating cold NSs [9,10], the current subset of models extended to finite temperature is much more limited, which allows us to focus on only a handful of different models. More precisely, the EOSs that fulfill our selection criteria (discussed in detail in the following sections) are the following: TNTYST [11] and SRO(APR) [12], both employing the same basic two-body Argonne V18 [13] and the three-body Urbana UIX [14,15] nuclear potentials and based on variational calculations as the original APR EOS [7], the Brueckner-Hartree-Fock (BHF) EOSs V18 and N93 [16][17][18][19], the covariant density-functional theory EOS models Shen11 [20,21] (based on TM1 [22]), Shen20 [23] (based * jinbiao.wei@ct.infn.it on TM1e [24]), HS(DD2) [25,26], SFH(SFHx) [25,27], and FSU2H [28,29].…”

Section: Introductionmentioning

confidence: 99%

“…As currently the finite-temperature sector of these EOSs is practically unaffected by observational constraints, they exhibit rather varying thermal behaviors. In particular, it has been noted [19,[37][38][39] that the predictions for the effects of temperature on stellar stability are widely varying: RMF and Skyrme-type models usually predict increasing stability (maximum gravitational mass) with temperature [37,40,41], whereas BHF results [18,19,[42][43][44][45] indicate in general a slight reduction of the maximum mass. We will try to analyze in some detail this phenomenon and try to establish a correlation with features of the EOS.…”

Section: Introductionmentioning

confidence: 99%

Hot neutron stars and their equation of state

Wei,

Burgio,

Raduta

et al. 2021

Preprint

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A set of microscopic, covariant density-functional, and non-relativistic Skyrme-type equations of state is employed to study the structure of purely nucleonic neutron stars at finite temperature. After examining the agreement with presently available astrophysical observational constraints, we find that the magnitude of thermal effects depends on the nucleon effective mass as well as on the stiffness of the cold equation of state. We evidence a fairly small but model-dependent effect of finite temperature on stellar stability that is correlated with the relative thermal pressure inside the star.

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Hot neutron stars with microscopic equations of state

Cited by 45 publications

References 98 publications

Nuclear matter at finite temperature and static properties of proto-neutron star

Nuclear matter at finite temperature and static properties of proto-neutron star

Neutron Stars and Gravitational Waves: The Key Role of Nuclear Equation of State

Hot neutron stars and their equation of state

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