Equation of State of the Stellar Matter

2006 ◽  
pp. 31-47
Keyword(s):  
Equation Of State ◽  
Stellar Matter

scholarly journals A comparative study of statistical models for nuclear equation of state of stellar matter

2013 ◽  
Vol 907 ◽  
pp. 13-54 ◽  
Author(s):  
N. Buyukcizmeci ◽  
A.S. Botvina ◽  
I.N. Mishustin ◽  
R. Ogul ◽  
M. Hempel ◽  
...  
Keyword(s):  
Equation Of State ◽  
Comparative Study ◽  
Statistical Models ◽  
Stellar Matter ◽  
Nuclear Equation Of State

Effects of strong magnetic fields in dense stellar matter

2013 ◽  
Vol 9 (S302) ◽  
pp. 439-440
Author(s):  
A. Lavagno ◽  
F. Lingua
Keyword(s):  
Equation Of State ◽  
Magnetic Fields ◽  
Degrees Of Freedom ◽  
Compact Star ◽  
Relativistic Equation ◽  
Bulk Properties ◽  
Strong Magnetic Fields ◽  
Stellar Matter ◽  
Nuclear Equation Of State

AbstractWe study the effects of strong magnetic fields in dense stellar matter within an effective relativistic equation of state with the inclusion of hyperons and Δ(1232)-isobar degrees of freedom. The effects of high magnetic field interactions significantly affect the nuclear equation of state and the macroscopic properties of the star. In this framework we investigate the role of the presence of the Δ-isobars degrees of freedom in structure and in the bulk properties of the compact star.

The Equation of State of Stellar Matter

2012 ◽  
pp. 151-161
Author(s):  
Rudolf Kippenhahn ◽  
Alfred Weigert ◽  
Achim Weiss
Keyword(s):  
Equation Of State ◽  
Stellar Matter

scholarly journals Delta Resonance Coupling with Walecka’s Mesons: Implications to Stellar Matter EoS

2017 ◽  
Vol 45 ◽  
pp. 1760034
Author(s):  
William Silva Gomes ◽  
José Carlos Teixeira de Oliveira ◽  
Hilário Rodrigues ◽  
Sérgio B. Duarte
Keyword(s):  
Phase Transition ◽  
Neutron Star ◽  
Equation Of State ◽  
Mean Field ◽  
Field Approximation ◽  
Coupling Constants ◽  
Mean Field Approximation ◽  
Stellar Matter ◽  
Baryonic Resonance ◽  
Resonance Coupling

In this work we have obtained the equation of state to the highly asymmetric dense stellar matter, using the nonlinear Walecka model in the mean field approximation. We discussed the implication of changes in coupling constant of the delta baryonic resonance on the observable of the neutron star. A detailed analysis of the equation of state and of the baryonic effective mass in respect to changes in the delta coupling constants is carried out. We focus attention on a new aspect observed for pressure when varying the baryonic density of the medium; a first order phase transition like a liquid-gas phase transition was observed for an acceptable range of delta coupled constant values. We have explored the implication of this aspect for the neutron star structure and their maximum masses.

NEUTRINO OPACITIES AND THE PASTA PHASE STRUCTURE

2011 ◽  
Vol 20 (supp01) ◽  
pp. 195-202
Author(s):  
DÉBORA PERES MENEZES ◽  
MARCELO DALLAGNOL ALLOY
Keyword(s):  
Equation Of State ◽  
Diffusion Coefficients ◽  
Phase Structure ◽  
Stellar Matter ◽  
The Mean ◽  
Protoneutron Stars

The diffusion coefficients that are related to the neutrino opacities are calculated in such a way that the formation of nuclear pasta and homogeneous matter at low densities are taken into account. Two methods are developed to build the pasta phase and their differences are outlined. One of them is chosen as part of a complete equation of state used in the calculation of the diffusion coefficients. Our results show that the mean free paths are significantly altered by the presence of nuclear pasta in stellar matter when compared with the results obtained with pure homogeneous matter. These differences in neutrino opacities will have consequences in the calculation of the Kelvin-Helmholtz phase of protoneutron stars.

Sign in / Sign up

Export Citation Format

Share Document