Implications of the Generalized Uncertainty Principle on the Walecka Model Equation of State and Neutron Star Structure

2021 ◽  
Author(s):  
Adrian G. Abac ◽  
Jose Perico H. Esguerra
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Uncertainty Principle ◽  
Model Equation ◽  
Generalized Uncertainty Principle ◽  
Walecka Model ◽  
Star Structure

scholarly journals COMPUTATION OF NEUTRON STAR STRUCTURE USING MODERN EQUATION OF STATE

2006 ◽  
Vol 21 (07) ◽  
pp. 1555-1565 ◽  
Author(s):  
G. H. BORDBAR ◽  
M. HAYATI
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Equations Of State ◽  
Maximum Mass ◽  
Neutron Star Matter ◽  
Radio Pulsars ◽  
Good Consistency ◽  
The Given ◽  
Neutron Star Radius ◽  
Star Structure

Using the modern equations of state derived from microscopic calculations, we have calculated the neutron star structure. For the neutron star, we have obtained a minimum mass about 0.1 M⊙ which is nearly independent of the equation of state, and a maximum mass between 1.47 M⊙ and 1.98 M⊙ which is strongly dependent on the equation of state. It is shown that among the equations of state of neutron star matter which we have used, the stiffest one leads to higher maximum mass and radius and lower central density. It is seen that the given maximum mass for the Reid-93 equation of state shows a good consistency with the accurate observations of radio pulsars. We have indicated that the thickness of neutron star crust is very small compared to the predicted neutron star radius.

scholarly journals The equation of state of neutron matter, symmetry energy and neutron star structure

2014 ◽  
Vol 50 (2) ◽  
Author(s):  
S. Gandolfi ◽  
J. Carlson ◽  
S. Reddy ◽  
A. W. Steiner ◽  
R. B. Wiringa
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Neutron Matter ◽  
Star Structure

scholarly journals A Study on Quark-Gluon Plasma Equation of State Using Generalized Uncertainty Principle

2013 ◽  
Vol 04 (04) ◽  
pp. 13-20 ◽  
Author(s):  
Nabil M. El Naggar ◽  
Lotfy I. Abou-Salem ◽  
Ibrahim A. Elmashad ◽  
Ahmed Farag Ali
Keyword(s):  
Equation Of State ◽  
Uncertainty Principle ◽  
Quark Gluon Plasma ◽  
Generalized Uncertainty Principle ◽  
Gluon Plasma ◽  
Plasma Equation

NEUTRON STAR MASS CORRELATION WITH SOUND VELOCITY AND INCOMPRESSIBILITY AT THE STAR CENTER IN THE POLYTROPIC APPROXIMATION

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1575-1582
Author(s):  
L. FERRARI ◽  
P. C. R. ROSSI ◽  
M. MALHEIRO
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Sound Velocity ◽  
Mean Field ◽  
Star Mass ◽  
Mean Field Models ◽  
Neutron Star Mass ◽  
Analytic Expressions ◽  
Walecka Model

In this paper we use a polytropic approximation to the equation of state for the interior of neutrons stars, described by relativistic hadronic mean field models. In this approximation, it is possible to obtain analytic expressions for the sound velocity and the incompressibility at the star center. We found a correlation between these quantities and the star mass. Using two well-known parametrizations of the nonlinear Walecka model for nuclear matter composed only of protons, neutrons and electron in β equilibrium, we obtain for a star mass of 1.43 M⊙ a central incompressibility Kc = (3000±100), around ten times the nuclear matter incompressibility, and a central sound velocity (v/c)2 ~ 0.3.

scholarly journals Neutron star structure with nuclear force mediated by hypothetical X17 boson

2021 ◽  
Vol 252 ◽  
pp. 04008
Author(s):  
Vlasios Petousis ◽  
Martin Veselský ◽  
Jozef Leja
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Force ◽  
Nuclear Equation Of State ◽  
Upper Limit ◽  
Merger Event ◽  
Star Structure

A reported 17 MeV boson, which has been proposed as an explanation to the 8Be and 4He anomaly, is investigated in the context of its possible influence to neutron stars structure. Implementing a mX =17 MeV to the nuclear equation of state using different incompressibility values K0=245 MeV and K0=260 MeV and solving Tolman-Oppenheimer-Volkoff equations, we estimate an upper limit of MTOV ≈ 2.4M⊙ for a non rotating neutron star with span in radius R between 11.5 km to 14 km. Moving away from pure -NN with admixture of 10% protons and simulating possible softening of equation of state due to hyperons, we see that our estimated limits fit quite well inside the newest reported studies, coming from neutron stars merger event, GW190814

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