High density matter
arXiv:1302.1928 · doi:10.1051/epjconf/20136303009
Abstract
The microscopic composition and properties of matter at super-saturation densities have been the subject of intense investigation for decades. The scarcity of experimental and observational data has lead to the necessary reliance on theoretical models. However, there remains great uncertainty in these models, which, of necessity, have to go beyond the over-simple assumption that high density matter consists only of nucleons and leptons. Heavy strange baryons, mesons and quark matter in different forms and phases have to be included to fulfil basic requirements of fundamental laws of physics. In this review the latest developments in construction of the Equation of State (EoS) of high-density matter at zero and finite temperature assuming different composition of the matter are surveyed. Critical comparison of model EoS with available observational data on neutron stars, including gravitational masses, radii and cooling patterns is presented. The effect of changing rotational frequency on the composition of neutron stars during their lifetime is demonstrated. Compatibility of EoS of high-density, low temperature compact objects and low density, high temperature matter created in heavy-ion collisions is discussed.
10 pages, 6 figures, Invited talk at Nuclei in Cosmos 2012, accepted for publication on PoS. arXiv admin note: text overlap with arXiv:1201.0950 by other authors
References in corpus (10)
- Color superconductivity in dense quark matter
- Cold Quark Matter
- Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter
- The Skyrme Interaction in finite nuclei and nuclear matter
- Astrophysical Measurement of the Equation of State of Neutron Star Matter
- Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12-25 M_sol Stars
- Symmetry energy of dilute warm nuclear matter
- Cold uniform matter and neutron stars in the quark-mesons-coupling model
- Chiral model approach to quark matter nucleation in neutron stars
- Relevance of equilibrium in multifragmentation