scholarly journals Neutron star properties and the nuclear equation of state

Astrophysics ◽  
10.5772/32054 ◽  
2012 ◽  
Author(s):  
Francesca Sammarruca
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Equation Of State

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 NEUTRON STAR VERSUS HEAVY-ION DATA: IS THE NUCLEAR EQUATION OF STATE HARD OR SOFT?

2008 ◽  
Author(s):  
JÜRGEN SCHAFFNER-BIELICH ◽  
IRINA SAGERT ◽  
MIRJAM WIETOSKA ◽  
CHRISTIAN STURM
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Heavy Ion ◽  
Nuclear Equation Of State ◽  
Star Versus

scholarly journals Rotation-Driven Phase Transitions in the Cores of Pulsars

2017 ◽  
Vol 45 ◽  
pp. 1760035
Author(s):  
Richard D. Mellinger ◽  
William Spinella ◽  
Fridolin Weber ◽  
Gustavo A. Contrera ◽  
Milva Orsaria
Keyword(s):  
Phase Transitions ◽  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Quark Matter ◽  
Nuclear Data ◽  
Particle Composition ◽  
Nuclear Equation Of State ◽  
The Impact ◽  
Gravitational Compression

In this paper, we discuss the impact of rotation on the particle composition of rotating neutron stars (pulsars). Particular emphasis is put on the formation of quark matter during stellar spin-down, driven by continuous gravitational compression. Our study is based on modern models for the nuclear equation of state whose parameters are tightly constrained by nuclear data, neutron star masses, and the latest estimates of neutron star radii.

CONSISTENT THREE-BODY FORCE WITH BONN B POTENTIAL AND NEUTRON STAR STRUCTURE

2010 ◽  
Vol 19 (08n09) ◽  
pp. 1727-1733 ◽  
Author(s):  
Z. H. LI ◽  
U. LOMBARDO ◽  
H.-J. SCHULZE ◽  
W. ZUO
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Body Force ◽  
Nucleon Force ◽  
Nucleon Potential ◽  
Saturation Properties ◽  
Nuclear Equation Of State ◽  
Neutron Star Mass ◽  
Three Body

Microscopic three-nucleon force consistent with the Bonn B two-nucleon potential is constructed, which includes Δ(1232), Roper, and nucleon-antinucleon excitation contributions. Recent results for the choice of the meson parameters are discussed. The forces are used in Brueckner calculations and the saturation properties of nuclear matter are determined. At the high densities, the nuclear equation of state and the symmetry energy are calculated. The corresponding neutron star mass-radius relations are presented.

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