Asymmetric Neutrino Production in Strongly Magnetized Proto-Neutron Stars

Abstract

We calculate the neutrino production cross-section through the direct URCA process in proto-neutron star matter in the presence of a strong magnetic field. We assume isoentropic conditions and introduce a new equation of state parameter-set in the relativistic mean-field approach that can reproduce neutron stars with $M>1.96$ M${}_{\odot }$ as required by observations. We find that the production process increases the flux of emitted neutrinos along the direction parallel to the magnetic field and decreases the flux in the opposite direction. This means that the neutrino flux asymmetry due to the neutrino absorption and scattering processes in a magnetic field becomes larger by the inclusion of the neutrino production process.

9 pages, 3 figures

References in corpus (7)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
• Constraining hypernuclear density functional with $\Lambda$-hypernuclei and compact stars
• Asymmetric neutrino propagation in newly born magnetized strange stars: GRB and kicks
• Pulsar Kicks With Modified URCA and Electrons in Landau Levels
• Supernovae, Landau Levels, and Pulsar Kicks