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On the appearance of hyperons in neutron stars

By employing a recently constructed hyperon-nucleon potential the equation of state of β-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.

preprint2010arXivOpen access
Haris DjapoBernd-Jochen SchaeferJochen Wambach
astro-phhep-phnucl-thhep-th
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Haris DjapoBernd-Jochen SchaeferJochen Wambach

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