2002/12/31 by D. Guetta, Dafne Guetta, Jonathan Granot · 30 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Gamma-ray burst #Gamma-ray bursts and supernovae #Neutrino #Nuclear physics #Physics #Pulsar #Pulsars and Gravitational Waves Research #Supernova #astro-ph #hep-ph
paper · pdf · doi:10.1103/physrevlett.90.201103
published in Physical Review Letters 90(20), 201103 (American Physical Society) · Accepted for publication in PRL. 4 pages, 3 figures, minor changes
arxiv created 2003/04/22 · openalex publication_date 2003/05/22 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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.