Propagation and Neutrino Oscillations in the Base of a Highly Magnetized Gamma-Ray Burst Fireball Flow

Abstract

Neutrons play an important role in the dynamics of gamma-ray bursts. The presence of neutrons in the baryon-loaded fireball is expected. If the neutrons abundance is comparable to that of protons, important features may be observed such as quasithermal multi-GeV neutrinos in coincidence with a subphotospheric γ-ray emission, nucleosynthesis at later times and rebrightening of the afterglow emission. Additionally, thermal MeV neutrinos are created by electron-positron annihilation, electron (positron) capture on protons (neutrons) and nucleonic bremsstrahlung. Although MeV neutrinos are difficult to detect, quasi-thermal GeV neutrinos are expected in km 3 detectors and/or DeepCore+IceCube. In this paper, we show that neutrino oscillations have outstanding implications for the dynamics of the fireball evolution and also that they can be detected through their flavor ratio on Earth. For that we derive the resonance and charged-neutrality conditions as well as the neutrino self-energy and effective potential up to order m −4 W at strong, moderate and weak magnetic field approximation to constrain the dynamics of the fireball. We found important implications: i) resonant oscillations are suppressed for high baryon densities as well as neutrons abundance larger than that of protons and ii) the effect of magnetic field is to decrease the proton-to-neutron ratio aside from the number of multi-GeV neutrinos expected in DeepCore detector. Also we estimate the GeV neutrino flavor ratios along the jet and on Earth.

Could a Hypercritical Accretion be Associated with the Atypical Magnetic-field Behavior in RX J0822-4300?

“…Weak B-field limit -In the weak B-field approximation, the effective potential does not depend on the Landau levels. Therefore, it can be written as (Fraija 2014b)…”

Observation of Radio Galaxies with HAWC

“…Photo hadronic interactions in the emitting region also generate neutrinos through the charged pion decay products (π ± → µ ± + ν µ /ν µ → e ± + ν µ /ν µ +ν µ /ν µ + ν e /ν e ). Taking into account the distance of M87, the neutrino flux ratio (1 : 2 : 0 ) created on the source will arrive on the standard ratio (1 : 1 : 1 ) [24,25]. The neutrino spectrum produced by the photo hadronic interactions is 8) where the factor A ν normalized through the TeV γ-ray flux is…”

Could a plasma in quasi-thermal equilibrium be associated to the “orphan” TeV flares?

“…This resonance depends on the effective potential and neutrino oscillation parameters. The equations that determine the neutrino evolution in matter for two and three flavors are related as follows [27,56].…”

“…We have studied the active-active neutrino process in the Wein fireball. We have used the neutrino effective potential at the weak field limit obtained by Fraija [27]. It depends on temperature (θ), chemical potential (µ), magnetic field (B) and neutrino energy (E ν ) for N e =N e (eq.…”