Neutrinos from Gamma-Ray Bursts in Pulsar Wind Bubbles: \sim 10^{16} eV

Details Neutrinos from Gamma-Ray Bursts in Pulsar Wind Bubbles: \sim 10^{16} eV Neutrinos from Gamma-Ray Bursts in Pulsar Wind Bubbles: \sim 10^{16} eV

2002-12-02

arxiv.org/abs/astro-ph/0212045v2

Phys.Rev.Lett.90:201103,2003

Astronomy and Astrophysics

Astrophysics

Accepted for publication in PRL. 4 pages, 3 figures, minor changes

Scientific paper

10.1103/PhysRevLett.90.201103

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 \sim 10^{16} eV neutrinos. A km^2 neutrino detector would observe several events per year correlated with the GRBs.

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