Enhancement of the ${\bar{\nu }}_e$ flux from astrophysical sources by two photon annihilation interactions

Abstract

The ratio of anti-electron to total neutrino flux, ${\Phi }_{{\bar{\nu }}_e}:{\Phi }_{\nu }$, expected from $p\gamma$ interactions in astrophysical sources is $\le 1:15$. We point out that this ratio is enhanced by the decay of ${\mu }^{+}{\mu }^{-}$ pairs, created by the annihilation of secondary high energy photons from the decay of the neutral pions produced in $p\gamma$ interactions. We show that, under certain conditions, the ${\Phi }_{{\bar{\nu }}_e}:{\Phi }_{\nu }$ ratio may be significantly enhanced in gamma-ray burst (GRB) fireballs, and that detection at the Glashow resonance of ${\bar{\nu }}_e$ in kilometer scale neutrino detectors may constrain GRB fireball model parameters, such as the magnetic field and energy dissipation radius.

arXiv comment6 pages, 3 figures, PRD accepted

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Cited by in corpus (8)

• Flavor Ratios of Astrophysical Neutrinos: Implications for Precision Measurements
• Astrophysical tau neutrino detection in kilometer-scale Cherenkov detectors via muonic tau decay
• Neutrino Astronomy with IceCube
• Neutrino Production in Electromagnetic Cascades: An extra component of cosmogenic neutrino at ultrahigh energies
• Neutrino emission from a GRB afterglow shock during an inner supernova shock breakout
• Neutrino production from photo-hadronic interactions of the gamma flux from Active Galactic Nuclei with their gas content
• Constraining Galactic $p\gamma$ Interactions with Cosmic Ray Electron and Positron Spectra
• Spread Complexity of High Energy Neutrino Propagation over Astrophysical Distances