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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Bibliographic Details
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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Summary: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.
ISSN:0556-2813
1089-490X
DOI:10.1103/PhysRevC.81.035803