Hypernuclear Physics for Neutron Stars
Abstract
The role of hypernuclear physics for the physics of neutron stars is delineated. Hypernuclear potentials in dense matter control the hyperon composition of dense neutron star matter. The three-body interactions of nucleons and hyperons determine the stiffness of the neutron star equation of state and thereby the maximum neutron star mass. Two-body hyperon-nucleon and hyperon-hyperon interactions give rise to hyperon pairing which exponentially suppresses cooling of neutron stars via the direct hyperon URCA processes. Non-mesonic weak reactions with hyperons in dense neutron star matter govern the gravitational wave emissions due to the r-mode instability of rotating neutron stars.
Cite
@article{arxiv.0801.3791,
title = {Hypernuclear Physics for Neutron Stars},
author = {Jurgen Schaffner-Bielich},
journal= {arXiv preprint arXiv:0801.3791},
year = {2009}
}
Comments
19 pages, 2 figures, updated and extended version of astro-ph/0703113, accepted for publication in a special issue of Nuclear Physics A `Recent Advances in Strangeness Nuclear Physics'