Neutrinos from individual gamma-ray bursts in the BATSE catalog

Abstract

We estimate the neutrino emission from individual gamma-ray bursts observed by the BATSE detector on the Compton Gamma-Ray Observatory. Neutrinos are produced by photoproduction of pions when protons interact with photons in the region where the kinetic energy of the relativistic fireball is dissipated allowing the acceleration of electrons and protons. We also consider models where neutrinos are predominantly produced on the radiation surrounding the newly formed black hole. From the observed redshift and photon flux of each individual burst, we compute the neutrino flux in a variety of models based on the assumption that equal kinetic energy is dissipated into electrons and protons. Where not measured, the redshift is estimated by other methods. Unlike previous calculations of the universal diffuse neutrino flux produced by all gamma-ray bursts, the individual fluxes (compiled at http://www.arcetri.astro.it/∼ dafne/grb/) can be directly compared with coincident observations by the AMANDA telescope at the South Pole. Because of its large statistics, our predictions are likely to be representative for future observations with larger neutrino telescopes.

Cosmic neutrinos from the sources of galactic and extragalactic cosmic rays

“…In this scenario the production of neutrinos of 100-1000 TeV energy in the GRB fireball is a robust prediction because neutrinos are inevitably produced in interactions of accelerated protons with fireball photons. Estimates of the flux [19] point again at the necessity of a kilometer-cubed neutrino detector, in agreement with the generic energetics estimates previously presented. Studies of active galaxies as sources of cosmic rays lead to similar conclusions [17].…”

“…AMANDA's sensitivity is within a factor of 2 of the most optimistic predictions. Also shown are fluxes predicted by specific models of cosmic ray accelerators: active galaxies labeled StSa [17] and MPR [18], GRB [19] and the diffuse flux produced by cosmic ray producing active galaxies on microwave photons[20] labelled RB. Data for the background atmospheric neutrino flux are from the AMANDA experiment.…”

High Energy Cosmic Ray and Neutrino Astronomy

“…Eq. (12) implies a detection rate of ∼ 10 neutrino-induced muon events per year (over 4π sr) in a 1 Gton (1 cubic-km) detector [13,28,49,77,100]. The upper limit on the GRB neutrino emission provided by the AMANDA (∼ 0.05 Gton) detector approaches the flux predicted by Eq.…”

Neutrinos from decaying muons, pions, neutrons and kaons in gamma ray bursts

“…For cosmic neutrinos with an E −2 energy spectrum an integral flux limit of E 2 φ ≤ 3.6 × 10 −8 GeV cm −2 sec −1 sr −1 has been found in the energy interval of 2 × 10 6 − 6.3 × 10 9 GeV [30]. In particular the non-detection of neutrinos from GRBs [32] has placed a tighter upper bound which is 3.7 times below the theoretical predictions [7,8,11,26] combining 40 and 59 strings. IceCube collaboration has concluded [32] that GRBs are not the only sources of cosmic rays above energy 1 EeV or the efficiency of neutrino production is much lower than the current predictions.…”