Neutrinos of energy approximately 10(16) eV from gamma-ray bursts in pulsar wind bubbles.
The supranova model for gamma-ray bursts (GRBs) is becoming increasingly more popular. In this scenario the GRB occurs weeks to years after a supernova explosion, and is located inside a pulsar wind bubble (PWB). Protons accelerated in the internal shocks that emit the GRB may interact with the external PWB photons producing pions which decay into approximately 10(16) eV neutrinos. A km(2) neutrino detector would observe several events per year correlated with the GRBs.
Guetta
Dafne
D
Osservatorio astrofisico di Arcetri, Fermi 5, 50125 Firenze, Italy. dafne@arcetri.astro.it
Granot
Jonathan
J