Status of neutrino astronomy

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dc.creatorBecker, Julia K.
dc.date2008-11-05
dc.date.accessioned2026-07-07T12:15:56Z
dc.date.available2026-07-07T12:15:56Z
dc.descriptionAstrophysical neutrinos can be produced in proton interactions of charged cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in balloon, satellite and air shower experiments every day, from below 1e9 eV up to macroscopic energies of 1e21 eV. The observation of different photon fields has been done ever since, today with detections ranging from radio wavelengths up to very high-energy photons in the TeV range. The leading question for neutrino astronomers is now which sources provide a combination of efficient proton acceleration with sufficiently high photon fields or baryonic targets at the same time in order to produce a neutrino flux that is high enough to exceed the background of atmospheric neutrinos. There are only two confirmed astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit and emitted neutrinos at MeV energies. The aim of large underground Cherenkov telescopes like IceCube and KM3NeT is the detection of neutrinos at energies above 100 GeV. In this paper, recent developments of neutrino flux modeling for the most promising extragalactic sources, gamma ray bursts and active galactic nuclei, are presented.
dc.descriptionTalk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4 figures, 1 table
dc.identifierhttps://arxiv.org/abs/0811.0696
dc.identifierhttp://arxiv.org/abs/0811.0696
dc.identifierJ.Phys.Conf.Ser.136:022055,2008
dc.identifierdoi:10.1088/1742-6596/136/2/022055
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/211647
dc.subjectAstrophysics
dc.titleStatus of neutrino astronomy
dc.typetext

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