Updates of the nuclear equation of state for core-collapse supernovae and neutron stars: effects of 3-body forces, QCD, and magnetic fields

International Symposium on Exotic Nuclear Structure From Nucleons 2012

Mathews, G.J.^1 ; Meixner, M.^1 ; Olson, J.P.^1 ; Suh, I.-S.^1 ; Kajino, T.^2 ; Maruyama, T.^3 ; Hidaka, J.^2 ; Ryu, C.-Y.^4 ; Cheoun, M.-K.^5 ; Lan, N.Q.^6

Department of Physics, Center for Astrophysics, University of Notre Dame, Notre Dame, IN, United States^1

Theory Division, National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan^2

College of Bioresource Sciences, Nihon University, Fujisawa 252-8510, Japan^3

General Education Curriculum Center, Hanyang University, Seoul 133-791, Korea, Republic of^4

Department of Physics, Soongsil University, Seoul, Korea, Republic of^5

Hanoi National University of Education, 136 Xuan Thuy, Hanoi, Viet Nam^6

关键词: Absorption cross sections;    Core collapse supernovae;    Magnetized neutron stars;    Nuclear equation of state;    Perturbative calculations;    Scattering and absorption;    Strong magnetic fields;    Supernova simulations;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/445/1/012023/pdf
DOI  :  10.1088/1742-6596/445/1/012023

来源: IOP

【 摘 要 】

We summarize several new developments in the nuclear equation of state for supernova simulations and neutron stars. We discuss an updated and improved Notre-Dame-Livermore Equation of State (NDL EoS) for use in supernovae simulations. This Eos contains many updates. Among them are the effects of 3- body nuclear forces at high densities and the possible transition to a QCD chiral and/or super-conducting color phase at densities. We also consider the neutron star equation of state and neutrino transport in the presence of strong magnetic fields. We study a new quantum hadrodynamic (QHD) equation of state for neutron stars (with and without hyperons) in the presence of strong magnetic fields. The parameters are constrained by deduced masses and radii. The calculated adiabatic index for these magnetized neutron stars exhibit rapid changes with density. This may provide a mechanism for star-quakes and flares in magnetars. We also investigate the strong magnetic field effects on the moments of inertia and spin down of neutron stars. The change of the moment of inertia associated with emitted magnetic flares is shown to match well with observed glitches in some magnetars. We also discuss a perturbative calculation of neutrino scattering and absorption in hot and dense hyperonic neutron-star matter in the presence of a strong magnetic field. The absorption cross-sections show a remarkable angular dependence in that the neutrino absorption strength is reduced in a direction parallel to the magnetic field and enhanced in the opposite direction. The pulsar kick velocities associated with this asymmetry comparable to observed pulsar velocities and may affect the early spin down rate of proto-neutron star magnetars with a toroidal field configuration.