scholarly journals Nuclear equation of state at high density and the properties of neutron stars

2000 ◽  
Vol 62 (4) ◽  
Author(s):  
P. K. Sahu
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
High Density ◽  
Nuclear Equation Of State

scholarly journals Chiral Effective Field Theory and the High-Density Nuclear Equation of State

2021 ◽  
Vol 71 (1) ◽  
Author(s):  
C. Drischler ◽  
J.W. Holt ◽  
C. Wellenhofer
Keyword(s):  
Field Theory ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Effective Field Theory ◽  
Effective Field ◽  
High Density ◽  
Chiral Effective Field Theory ◽  
Nuclear Equation Of State ◽  
Density Regime

Born in the aftermath of core-collapse supernovae, neutron stars contain matter under extraordinary conditions of density and temperature that are difficult to reproduce in the laboratory. In recent years, neutron star observations have begun to yield novel insights into the nature of strongly interacting matter in the high-density regime where current theoretical models are challenged. At the same time, chiral effective field theory has developed into a powerful framework to study nuclear matter properties with quantified uncertainties in the moderate-density regime for modeling neutron stars. In this article, we review recent developments in chiral effective field theory and focus on many-body perturbation theory as a computationally efficient tool for calculating the properties of hot and dense nuclear matter. We also demonstrate how effective field theory enables statistically meaningful comparisons among nuclear theory predictions, nuclear experiments, and observational constraints on the nuclear equation of state. Expected final online publication date for the Annual Review of Nuclear and Particle Science, Volume 71 is September 2021. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

EFFECTS OF THE NUCLEAR SYMMETRY ENERGY ON GRAVITATIONAL WAVES FROM THE AXIAL W-MODES OF ISOLATED NEUTRON STARS

2010 ◽  
Vol 19 (08n09) ◽  
pp. 1712-1719
Author(s):  
DE-HUA WEN ◽  
BAO-AN LI ◽  
PLAMEN G. KRASTEV
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
Symmetry Energy ◽  
Laboratory Data ◽  
High Density ◽  
Nuclear Symmetry Energy ◽  
Nuclear Equation Of State ◽  
Eigen Frequencies ◽  
Density Behavior

The frequencies and damping times of the axial w-mode oscillations of neutron stars are investigated using a nuclear equation of state (EOS) partially constrained by the available terrestrial laboratory data. It is found that the nuclear symmetry energy E sym (ρ), especially its high density behavior, plays an important role in determining both the eigen-frequencies and the damping times of these oscillations.

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.

scholarly journals QCD at high density: Equation of state for nuclear collisions and neutron stars

2019 ◽  
Vol 982 ◽  
pp. 891-894 ◽  
Author(s):  
Anton Motornenko ◽  
Volodymyr Vovchenko ◽  
Jan Steinheimer ◽  
Stefan Schramm ◽  
Horst Stoecker
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
High Density ◽  
Nuclear Collisions ◽  
Density Equation

scholarly journals How neutron stars constrain the nuclear equation of state

2014 ◽  
Vol 66 ◽  
pp. 04011
Author(s):  
Thomas Hell ◽  
Bernhard Röttgers ◽  
Wolfram Weise
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Equation Of State

THE BETHE–BRUECKNER–GOLDTONE THEORY OF THE NUCLEAR EQUATION OF STATE AND NEUTRON STARS

2003 ◽  
Vol 17 (28) ◽  
pp. 5127-5137 ◽  
Author(s):  
M. BALDO ◽  
G. F. BURGIO
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Gluon Plasma ◽  
Many Body ◽  
Static Properties ◽  
Many Body Theory ◽  
Nuclear Equation Of State ◽  
Pure Neutron Matter ◽  
Particle Potential ◽  
Three Body

The microscopic many-body theory of the Nuclear Equation of State is discussed in the framework of the Bethe–Brueckner–Goldstone method. The expansion is extended up to the three hole-line diagrams contribution. The Brueckner equation for the two-body G-matrix and the Bethe–Fadeev equation for the three-body scattering matrix are solved both for the gap and continuous choices of the single particle potential. For symmetric and pure neutron matter strong evidence of convergence in the expansion is found. Once three-body forces are introduced, the phenomenological saturation point is reproduced. In order to study neutron stars static properties, the theory is extended to include strangeness, and the possible quark-gluon plasma component is described in the simplified MIT bag model. The results for the mass and radius of neutron stars are briefly discussed.

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