Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2012-02-26
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
20 pages, 9 figures; to appear as a chapter in the book "Neutron Star Crust", edited by C. A. Bertulani and J. Piekarewicz
Scientific paper
Physics of the Equation of State (EoS) for proto-neutron star (PNS) concerns properties of neutron rich matter at finite temperature over wide range of densities. In this contribution we discuss the structure of PNS inner crust in a relativisitc mean filed model with spherical Wigner-Setiz approximation, and the composition of matter around neutrino-sphere in PNS in a virial expansion of non-ideal gas composed of nucleons and nuclei. We go on to discuss several new complete EoS for PNS and supernova, whose detailed composition is important for the neutrino dynamics. We focus on one important distinction for various EoS - the density dependence of symmetry energy E'sym, and its interesting correlation with the radii of neutron star, as well as properties of neutron distribution in neutron rich nuclei. Improved understanding of E'sym from terrestrial experiment on neutron distribution of neutron rich nuclei, benchmark calculations via ab initio methods, and statistical analysis on good quality observational data will advance our knowledge on EoS.
No associations
LandOfFree
Equation of State for Proto-Neutron Star does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Equation of State for Proto-Neutron Star, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Equation of State for Proto-Neutron Star will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-261818