Neutrino diffusion and mass ejection in protoneutron stars
- Universidade Federal do Acre-Campus Floresta, Estrada do Canela Fina, km 12, 69980-000, Cruzeiro do Sul, AC (Brazil)
- Centro Federal de Educacao Tecnologica do Rio de Janeiro, Av. Maracana 249, 20271-110, Rio de Janeiro, RJ (Brazil)
- Centro Brasileiro de Pesquisas Fisicas, Rua Dr. Xavier Sigaud 150, 22290-180, Rio de Janeiro, RJ (Brazil)
We discuss the mass ejection mechanism induced by diffusion of neutrino during the early stage of the protoneutron star cooling. A dynamical calculation is employed in order to determine the amount of matter ejected and the remnant compact object mass. An equation of state considering hadronic and quark phases for the stellar dense matter was used to solve the whole time evolution of the system during the cooling phase. The initial neutrino population was obtained by considering beta equilibrium in the dense stellar matter with confined neutrinos, in the very early period of the deleptonic stage of the nascent pulsar. For specified initial configurations of the protoneutron star, we solve numerically the set of equations of motion together with neutrino diffusion through the dense stellar medium.
- OSTI ID:
- 21503662
- Journal Information:
- Physical Review. D, Particles Fields, Vol. 82, Issue 10; Other Information: DOI: 10.1103/PhysRevD.82.105011; (c) 2010 American Institute of Physics; ISSN 0556-2821
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
CONFIGURATION
COOLING
DIFFUSION
EQUATIONS OF MOTION
EQUATIONS OF STATE
EQUILIBRIUM
EVOLUTION
HADRONS
MASS
NEUTRINOS
NEUTRON STARS
PULSARS
QUARKS
STARS
COSMIC RADIO SOURCES
DIFFERENTIAL EQUATIONS
ELEMENTARY PARTICLES
EQUATIONS
FERMIONS
LEPTONS
MASSLESS PARTICLES
PARTIAL DIFFERENTIAL EQUATIONS