Abstract
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.
Highlights
IntroductionThe high production of delta-resonances in the dense phase (ρ ≥ 3ρ0) of relativistic heavy ion collisions [1,2], where ρ0 is the normal nuclear matter density, leads to a
The high production of delta-resonances in the dense phase (ρ ≥ 3ρ0) of relativistic heavy ion collisions [1,2], where ρ0 is the normal nuclear matter density, leads to aThis is an Open Access article published by World Scientific Publishing Company
We discussed the implication of changes in coupling constant of the delta baryonic resonance on the observable of the neutron star
Summary
The high production of delta-resonances in the dense phase (ρ ≥ 3ρ0) of relativistic heavy ion collisions [1,2], where ρ0 is the normal nuclear matter density, leads to a. This is an Open Access article published by World Scientific Publishing Company. In this work we obtained the equation of state of baryons and leptons to the highly asymmetric dense stellar matter. Is the Lagrangian density for free baryons, free leptons (e−, μ−), and the meson fields σ, ωμ and ρμ. The interaction Lagrangian density is given by the following expression
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