scholarly journals Pairing effects in nuclear pasta phase within the relativistic Thomas-Fermi formalism

2021 ◽  
Author(s):  
Ubiratãn José Furtado ◽  
Sidney dos Santos Avancini ◽  
José Ricardo Marinelli
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Early Stage ◽  
Supernova Explosion ◽  
Pairing Force ◽  
Thomas Fermi ◽  
Seitz Cell ◽  
Protoneutron Star

Abstract Pairing effects in non-uniform nuclear matter, surrounded by electrons, are studied in the protoneutron star early stage and in other conditions. The so-called nuclear pasta phases at sub saturation densities are solved in a Wigner-Seitz cell, within the Thomas-Fermi approximation. The solution of this problem is important for the understanding of the physics of a newly born neutron star after a supernova explosion. It is shown that the pasta phase is more stable than uniform nuclear matter on some conditions and the pairing force relevance is studied in the determination of these stable phases.

A NUCLEAR MANY-BODY THEORY AT FINITE TEMPERATURE APPLIED TO A PROTONEUTRON STAR

2002 ◽  
Vol 11 (02) ◽  
pp. 83-104 ◽  
Author(s):  
GUILHERME F. MARRANGHELLO ◽  
CESAR A. Z. VASCONCELLOS ◽  
MANFRED DILLIG ◽  
J. A. DE FREITAS PACHECO
Keyword(s):  
Phase Transition ◽  
Nuclear Matter ◽  
Finite Temperature ◽  
Degrees Of Freedom ◽  
Many Body ◽  
Many Body Theory ◽  
The Masses ◽  
Protoneutron Stars ◽  
Protoneutron Star

Thermodynamical properties of nuclear matter are studied in the framework of an effective many-body field theory at finite temperature, considering the Sommerfeld approximation. We perform the calculations by using the nonlinear Boguta and Bodmer model, extended by the inclusion of the fundamental baryon octet and leptonic degrees of freedom. Trapped neutrinos are also included in order to describe protoneutron star properties through the integration of the Tolman–Oppenheimer–Volkoff equations, from which we obtain, beyond the standard relations for the masses and radii of protoneutron stars as functions of the central density, new results of these quantities as functions of temperature. Our predictions include: the determination of an absolute value for the limiting mass of protoneutron stars; new structural aspects on the nuclear matter phase transition via the behavior of the specific heat and, through the inclusion of quark degrees of freedom, the properties of a hadron-quark phase transition and hybrid protoneutron stars

scholarly journals Neutron Star Properties: Quantifying the Effect of the Crust–Core Matching Procedure

Universe ◽  
2020 ◽  
Vol 6 (11) ◽  
pp. 220
Author(s):  
Márcio Ferreira ◽  
Constança Providência
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Strong Impact ◽  
The Core ◽  
Meta Modeling ◽  
Low Mass ◽  
Matching Procedure ◽  
The Impact

The impact of the equation of state (EoS) crust-core matching procedure on neutron star (NS) properties is analyzed within a meta-modeling approach. Using a Taylor expansion to parametrize the core equation of state (EoS) and the SLy4 crust EoS, we create two distinct EoS datasets employing two matching procedures. Each EoS describes cold NS matter in a β equilibrium that is thermodynamically stable and causal. It is shown that the crust-core matching procedure affects not only the crust-core transition but also the nuclear matter parameter space of the core EoS, and thus the most probable nuclear matter properties. An uncertainty of as much as 5% (8%) on the determination of low mass NS radii (tidal deformability) is attributed to the complete matching procedure, including the effect on core EoS. By restricting the analysis, imposing that the same set of core EoS is retained in both matching procedures, the uncertainty on the NS radius drops to 3.5% and below 1.5% for 1.9M⊙. Moreover, under these conditions, the crust-core matching procedure has a strong impact on the Love number k2, of almost 20% for 1.0M⊙ stars and 7% for 1.9M⊙ stars, but it shows a very small impact on the tidal deformability Λ, below 1%.

scholarly journals Properties and Synthesis of Heavy Nuclei and Properties of Neutron Star Matter

1974 ◽  
Vol 53 ◽  
pp. 67-75
Author(s):  
J. Robert Buchler
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Superheavy Nuclei ◽  
Heavy Nuclei ◽  
Neutron Star Matter ◽  
Fermi Model ◽  
Bulk Properties ◽  
Properties Of Nuclei ◽  
Thomas Fermi

The nuclear Thomas-Fermi model which is based on nuclear matter calculations has been successfully applied to the study of the bulk properties of nuclei. It is ideally suited for extrapolation into the region of very neutron-rich and of superheavy nuclei. It is therefore a valuable approach for r-process calculations as well as for the study of neutron star matter at subnuclear densities.

ON COMPRESSED NUCLEAR MATTER: FROM NUCLEI TO NEUTRON STARS

2011 ◽  
Vol 20 (10) ◽  
pp. 1789-1796 ◽  
Author(s):  
JORGE A. RUEDA ◽  
M. ROTONDO ◽  
R. RUFFINI ◽  
S.-S. XUE
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
White Dwarfs ◽  
Traditional Approach ◽  
Equilibrium Equations ◽  
Fermi Model ◽  
Thomas Fermi ◽  
General Relativistic ◽  
The Way

We address the description of neutron-proton-electron degenerate matter in beta equilibrium subjected to compression both in the case of confined nucleons into a nucleus as well as in the case of deconfined nucleons. We follow a step-by-step generalization of the classical Thomas–Fermi model to special and general relativistic regimes, which leads to a unified treatment of beta equilibrated neutron-proton-electron degenerate matter applicable from the case of nuclei all the way up to the case of white-dwarfs and neutron stars. New gravito-electrodynamical effects, missed in the traditional approach for the description of neutron star configurations, are found as a consequence of the new set of general relativistic equilibrium equations.

Constraints on Estimation of Radius of Double Pulsar PSR J0737-3039A and Its Neutron Star Nuclear Matter Composition

2017 ◽  
Vol 34 (12) ◽  
pp. 129701 ◽  
Author(s):  
Yi-Yan Yang ◽  
Li Chen ◽  
Rong-Feng Linghu ◽  
Li-Yun Zhang ◽  
Ali Taani
Keyword(s):  
Neutron Star ◽  
Nuclear Matter

Protoneutron Star Formation

1988 ◽  
Vol 7 (4) ◽  
pp. 371-381
Author(s):  
Adam Burrows
Keyword(s):  
Star Formation ◽  
Neutron Star ◽  
General Analysis ◽  
Sn 1987A ◽  
Supernova Neutrino ◽  
Neutrino Theory ◽  
Protoneutron Star

AbstractThe theory of neutron star formation is addressed in the light of the detected neutrino burst from SN 1987A. A brief review of how supernova neutrino theory has evolved over the last 30 years and a general analysis of the SN 1987A detections is presented.

scholarly journals Nuclear equation of state and neutron star cooling

2017 ◽  
Vol 26 (04) ◽  
pp. 1750015 ◽  
Author(s):  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Evolution ◽  
Observation Data ◽  
Nuclear Equation Of State ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Nuclear Models

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models of dense nuclear matter. We focus on the effects of uncertainties originated from the nuclear models, the composition of elements in the envelope region, and the formation of superfluidity in the core and the crust of neutron stars. Discovery of [Formula: see text] neutron stars PSR J1614−2230 and PSR J0343[Formula: see text]0432 has triggered the revival of stiff nuclear equation of state at high densities. In the meantime, observation of a neutron star in Cassiopeia A for more than 10 years has provided us with very accurate data for the thermal evolution of neutron stars. Both mass and temperature of neutron stars depend critically on the equation of state of nuclear matter, so we first search for nuclear models that satisfy the constraints from mass and temperature simultaneously within a reasonable range. With selected models, we explore the effects of element composition in the envelope region, and the existence of superfluidity in the core and the crust of neutron stars. Due to uncertainty in the composition of particles in the envelope region, we obtain a range of cooling curves that can cover substantial region of observation data.

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