6533b851fe1ef96bd12a8f64
RESEARCH PRODUCT
Nuclear liquid-gas phase transition and supernovae evolution
Patrick BlottiauJérôme MargueronJesús Navarrosubject
Shock waveNuclear and High Energy PhysicsPhase transition97.60.Bw; 26.50.+x; 25.30.Pt; 21.60.JzNuclear Theory[PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th]supernovaeAstrophysics::High Energy Astrophysical PhenomenaNuclear TheoryFOS: Physical sciencesTrappingAstrophysics7. Clean energy01 natural sciencesNuclear Theory (nucl-th)Nuclear physics[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]0103 physical sciences010306 general physicsPhysics[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]010308 nuclear & particles physicsLiquid gasAstrophysics (astro-ph)FísicaneutrinosNuclear matterSupernovaphase transitionnuclear matterParticleNeutrinodescription
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.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2004-01-26 |