Appearance of hyperons in neutron stars

By employing a recently constructed hyperon-nucleon potential the equation of state of {beta}-equilibrated and charge neutral nucleonic matter is calculated. The hyperon-nucleon potential is a low-momentum potential which is obtained within a renormalization group framework. Based on the Hartree-Foc...

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Published in:Physical review. C, Nuclear physics Nuclear physics, 2010-03, Vol.81 (3), Article 035803
Main Authors: Ðapo, H., Schaefer, B.-J., Wambach, J.
Format: Article
Language:English
Subjects:
APPROXIMATIONS
BARYONS
CALCULATION METHODS
DENSITY
ELEMENTARY PARTICLES
EQUATIONS
EQUATIONS OF STATE
FERMIONS
HADRONS
HARTREE-FOCK METHOD
HYPERONS
MASS
MATTER
NEUTRON STARS
NUCLEAR MATTER
NUCLEAR PHYSICS AND RADIATION PHYSICS
NUCLEONS
PHYSICAL PROPERTIES
POTENTIALS
RENORMALIZATION
STARS
STRANGE PARTICLES
TEMPERATURE ZERO K
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description By employing a recently constructed hyperon-nucleon potential the equation of state of {beta}-equilibrated and charge neutral nucleonic matter is calculated. The hyperon-nucleon potential is a low-momentum potential which is obtained within a renormalization group framework. Based on the Hartree-Fock approximation at zero temperature the densities at which hyperons appear in neutron stars are estimated. For several different bare hyperon-nucleon potentials and a wide range of nuclear matter parameters it is found that hyperons in neutron stars are always present. These findings have profound consequences for the mass and radius of neutron stars.
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subjects APPROXIMATIONS
BARYONS
CALCULATION METHODS
DENSITY
ELEMENTARY PARTICLES
EQUATIONS
EQUATIONS OF STATE
FERMIONS
HADRONS
HARTREE-FOCK METHOD
HYPERONS
MASS
MATTER
NEUTRON STARS
NUCLEAR MATTER
NUCLEAR PHYSICS AND RADIATION PHYSICS
NUCLEONS
PHYSICAL PROPERTIES
POTENTIALS
RENORMALIZATION
STARS
STRANGE PARTICLES
TEMPERATURE ZERO K
title Appearance of hyperons in neutron stars
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