Hypernuclear Physics for Neutron Stars
By J. Schaffner-Bielich. 2008
157 citations recorded by the source corpus.
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. Nonmesonic weak reactions with hyperons in dense neutron star matter govern the gravitational wave emissions due to the r-mode instability of rotating neutron stars.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Geophysics
View Paper: https://www.semanticscholar.org/paper/8ada2b1b5c6cba0f54c89d4eb9dfcec1114a0e75
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In Astronomy and Astrophysics
In Atomic and Molecular Physics, and Optics
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Citations in the corpus
- Thermonuclear Burst Oscillations (2012, background): “A neutron star with a submillisecond spin period would place a tight and very clean constraint on the dense matter equation of state (Lattimer & Prakash 2007, Schaffner-Bielich 2008, Haensel et al. 2009).”