Signatures ofγray bursts in neutrino telescopes

Abstract

We show that the detection of neutrinos from a typical ␥ ray burst requires a kilometer-scale detector. We argue that large bursts should be visible with the neutrino telescopes under construction. We emphasize the three techniques by which neutrino telescopes can perform this search: by triggering on ͑i͒ bursts of muons from muon neutrinos, ͑ii͒ muons from air cascades initiated by high energy ␥ rays and ͑iii͒ showers made by relatively low energy (Ӎ100 MeV͒ electron neutrinos. The timing of neutrino-photon coincidences may yield a measurement of the neutrino mass to order 10 Ϫ4 -10 Ϫ5 eV. ͓S0556-2821͑96͒01616-5͔PACS number͑s͒: 95.55.Fw

Search for a possible space-time correlation between high energy neutrinos and gamma-ray bursts

“…for the upward-going muon flux are 0.87 10 −9 cm −2 (1.44 10 −9 cm −2 ) upward-going muons per average burst. These limits exclude an extreme cosmic string-type model reported in (Halzen 1996), which results in 10 −1 µ cm −2 , while according to a fireball scenario model in (Waxman 1997), a burst at a distance of 100 Mpc producing 0.4 10 51 erg in neutrinos of around 10 14 eV would produce ∼ 6 10 −11 cm −2 upward-going muons.…”

“…GRBs are possible sources of high energy νs: in the fireball scenario the beam dump mechanism can lead to ν emission (Halzen 1996;Waxman 1997). The short time duration of the GRB emission allows to reduce the atmospheric neutrino background thanks to the additional requirement on time coincidence with the GRB emission besides the directional coincidence.…”

The effect of neutrinos on the initial fireballs in gamma-ray bursts

“…The detectability of a neutrino source as described in this paper was studied by Halzen & Hooper (2002; see also Halzen, Jacobsen & Zas 1996; Halzen & Jaczko 1996). The detection is based on the charged current interaction and the subsequent Čerenkov radiation that is emitted by the positron.…”

Muon Detection of TeV Gamma Rays from Gamma‐Ray Bursts

“…We should here point out that MILAGRO, as well as the other instruments discussed, have other capabilities to study GRB. For instance, AMANDA has sensitivity to the MeV neutrinos produced in the initial collapse [10], and to neutrinos of TeV energy, and above [2]. The MILAGRO detector, beyond counting muons, can efficiently reconstruct gamma ray showers once their energy exceeds hundreds of GeV [8].…”