Nuclear liquid-gas phase transition and supernovae evolution
arXiv:astro-ph/0401545 · doi:10.1103/PhysRevC.70.028801
Abstract
It is shown that the large density fluctuations appearing at the onset of the first order nuclear liquid-gas phase transition can play an important role in the supernovae evolution. Due to these fluctuations, the neutrino gas may be trapped inside a thin layer of matter near the proto-neutron star surface. The resulting increase of pressure may induce strong particle ejection a few hundred milliseconds after the bounce of the collapse, contributing to the revival of the shock wave. The Hartree-Fock+RPA scheme, with a finite-range nucleon-nucleon effective interaction, is employed to estimate the effects of the neutrino trapping due to the strong density fluctuations, and to discuss qualitatively the consequences of the suggested new scenario.
version2 - precise that nuclear liquid-gas phase transition is 1st order and the unique instable mode is isoscalar
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- Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions
- Cluster formation in compact stars: relativistic versus Skyrme models
- Effective interaction dependence of the liquid-gas phase transition in symmetric nuclear matter
- Cluster formation in asymmetric nuclear matter: semi-classical and quantal approaches
- Anomalous thermodynamics and phase transitions of neutron-star matter
- Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations
- Phase transition towards strange matter
- Links Between Heavy Ion and Astrophysics
- Ising analogue to compact-star matter
- Pairing effects on neutrino transport in low-density stellar matter
- Energy and Angle Dependence of Neutrino Scattering Rates in Proto-Neutron Star and Supernova Matter within Skyrme RPA
- Dynamical response functions in correlated fermionic systems
- Charged Ising Model of Neutron Star Matter
- Phase diagram of neutron-rich nuclear matter and its impact on astrophysics
- Thermodynamics of compact-star matter within an ising approach
- Some aspects of the phase diagram of nuclear matter relevant to compact stars