Role of isospin physics in supernova matter and neutron stars
arXiv:1010.5856 · doi:10.1103/PhysRevC.82.055802
Abstract
We investigate the liquid-gas phase transition of hot protoneutron stars shortly after their birth following supernova explosion and the composition and structure of hyperon-rich (proto)neutron stars within a relativistic mean-field model where the nuclear symmetry energy has been constrained from the measured neutron skin thickness of finite nuclei. Light clusters are abundantly formed with increasing temperature well inside the neutrino-sphere for an uniform supernova matter. Liquid-gas phase transition is found to suppress the cluster yield within the coexistence phase as well as decrease considerably the neutron-proton asymmetry over a wide density range. We find symmetry energy has a modest effect on the boundaries and the critical temperature for the liquid-gas phase transition, and the composition depends more sensitively on the number of trapped neutrinos and temperature of the protoneutron star. The influence of hyperons in the dense interior of stars makes the overall equation of state soft. However, neutrino trapping distinctly delays the appearance of hyperons due to abundance of electrons. We also find that a softer symmetry energy further makes the onset of hyperon less favorable. The resulting structures of the (proto)neutron stars with hyperons and with liquid-gas phase transition are discussed.
arXiv comment11 pages, 7 figures, RevTex
References in corpus (30)
- The equation of state for nucleon matter and neutron star structure
- A New Parameterization for the Lagrangian Density of Relativistic Mean Field Theory
- Determination of the Equation of State of Dense Matter
- The Physics of Neutron Stars
- Neutron Star Observations: Prognosis for Equation of State Constraints
- Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions
- Isospin Asymmetry in Nuclei and Neutron Stars
- Composition and thermodynamics of nuclear matter with light clusters
- Neutron Star Structure and the Neutron Radius of 208Pb
- Composition and Structure of Protoneutron Stars
- Reaction Dynamics with Exotic Beams
- Neutron-Rich Nuclei in Heaven and Earth
- Evolution of Protoneutron Stars
- Nuclear symmetry energy probed by neutron skin thickness of nuclei
- Hyperon-rich Matter in Neutron Stars
- Determination of the stiffness of the nuclear symmetry energy from isospin diffusion
- Phase Transitions in Warm, Asymmetric Nuclear Matter
- In-medium nuclear interactions of low-energy hadrons
- Nuclear matter symmetry energy and the neutron skin thickness of heavy nuclei
- Equation of state of asymmetric nuclear matter and collisions of neutron-rich nuclei
- Evidence of Xi hypernuclear production in the ^{12}C(K^-,K^+)^{12}_{Xi}Be reaction
- Density dependence of the symmetry energy and the nuclear equation of state: A Dynamical and Statistical model perspective
- Constraining URCA cooling of neutron stars from the neutron radius of 208Pb
- Light nuclei quasiparticle energy shift in hot and dense nuclear matter
- Sensitivity of the Moment of Inertia of Neutron Stars to the Equation of State of Neutron-Rich Matter
- Formation of hot heavy nuclei in supernova explosions
- Liquid-Gas Phase Transition of Supernova Matter and Its Relation to Nucleosynthesis
- Liquid-gas phase transition and Coulomb instability of asymmetric nuclear systems
- Nuclear symmetry energy effects on liquid-gas phase transition in hot asymmetric nuclear matter
- Dynamical instabilities of warm matter: the meson effects
Cited by in corpus (5)
- Low density nuclear matter with light clusters in a generalized nonlinear relativistic mean-field model
- Effects of finite size and symmetry energy on the phase transition of stellar matter at subnuclear densities
- Cold dilute nuclear matter with -particle condensation in a generalized nonlinear relativistic mean-field model
- Effect of the Coulomb interaction on the liquid-gas phase transition of nuclear matter
- Finite temperature collective modes in a two phase coexistence region of asymmetric nuclear matter