scholarly journals High‐Density Skyrmion Matter and Neutron Stars

2008 ◽  
Vol 678 (1) ◽  
pp. 360-368 ◽  
Author(s):  
Prashanth Jaikumar ◽  
Manjari Bagchi ◽  
Rachid Ouyed
Keyword(s):  
Neutron Stars ◽  
High Density ◽  
Skyrmion Matter

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 Nuclear Forces in High Density Matter

1971 ◽  
Vol 46 ◽  
pp. 356-363
Author(s):  
M. R. McNaughton
Keyword(s):  
Neutron Stars ◽  
Nuclear Physics ◽  
High Density ◽  
Exclusion Principle ◽  
Nuclear Forces ◽  
Many Body ◽  
Simple Method ◽  
Preliminary Results ◽  
Future Developments ◽  
Density Matter

The conditions for superfluidity or ferromagnetism in neutron stars are presented and discussed (but not derived). It is suggested that present estimates relating to these are in error and that the predictions made contradict at least one of three sets of nuclear physics data cited in the text. This is due to neglecting the action of the exclusion principle.A comparatively simple method for calculating the strength of nuclear forces in the presence of many-body effects is outlined. Some preliminary results are presented together with projected future developments.

scholarly journals Constraining properties of high-density matter in neutron stars with magneto-elastic oscillations

2018 ◽  
Vol 476 (3) ◽  
pp. 4199-4212 ◽  
Author(s):  
Michael Gabler ◽  
Pablo Cerdá-Durán ◽  
Nikolaos Stergioulas ◽  
José A Font ◽  
Ewald Müller
Keyword(s):  
Neutron Stars ◽  
High Density ◽  
Density Matter

scholarly journals Density dependence of nuclear symmetry energy

2016 ◽  
Vol 31 (34) ◽  
pp. 1650194 ◽  
Author(s):  
B. Behera ◽  
T. R. Routray ◽  
S. K. Tripathy
Keyword(s):  
Neutron Stars ◽  
Density Dependence ◽  
Symmetry Energy ◽  
High Density ◽  
Nuclear Symmetry Energy ◽  
Density Behavior

High density behavior of nuclear symmetry energy is studied on the basis of the stiffest density dependence of asymmetric contribution to energy per nucleon in charge neutral n + p + e + [Formula: see text] matter under beta equilibrium. The density dependence of nuclear symmetry energy obtained in this way is neither very stiff nor soft at high densities and is found to be in conformity with recent observations of neutron stars.

High-density QCD phase transitions inside neutron stars: Glitches and gravitational waves

Pramana ◽  
2017 ◽  
Vol 89 (4) ◽  
Author(s):  
A M Srivastava ◽  
P Bagchi ◽  
A Das ◽  
B Layek
Keyword(s):  
Phase Transitions ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
High Density

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.

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