Abstract
We review the particle physics ingredients affecting the normalization, shape, and flavor composition of astrophysical neutrinos fluxes, such as different production modes, magnetic field effects on the secondaries (muons, pions, and kaons), and flavor mixing, where we focus onpγinteractions. We also discuss the interplay with neutrino propagation and detection, including the possibility to detect flavor and its application in particle physics, and the use of the Glashow resonance to discriminatepγfromppinteractions in the source. We illustrate the implications on fluxes and flavor composition with two different models: (1) the target photon spectrum is dominated by synchrotron emission of coaccelerated electrons and (2) the target photon spectrum follows the observed photon spectrum of gamma-ray bursts. In the latter case, the multimessenger extrapolation from the gamma-ray fluence to the expected neutrino flux is highlighted.
Highlights
In addition to gamma-ray and cosmic ray instruments, neutrino telescopes, such as IceCube 1 or ANTARES 2, provide interesting data on the sources of the highest-energetic particles found in the universe, so-called “cosmic accelerators”; see 3–6 for reviews
We focus on the minimal set of particle physics ingredients for the neutrino production, which must be present in virtually all sources, using several specific examples
In 74, the contribution of the different flavors to the cascade rate for a Eν−2 extragalactic test flux with equal contributions of all flavors at the Earth was given as electron neutrinos 40%, tau neutrinos 45%, and muon neutrinos 15% after all cuts. This implies that charged current showers dominate and that electron and tau neutrinos are detected with comparable efficiencies, that is, that 4.2 is a good first approximation to discuss flavor at a neutrino telescope
Summary
In addition to gamma-ray and cosmic ray instruments, neutrino telescopes, such as IceCube 1 or ANTARES 2 , provide interesting data on the sources of the highest-energetic particles found in the universe, so-called “cosmic accelerators”; see 3–6 for reviews. We focus on the minimal set of particle physics ingredients for the neutrino production, which must be present in virtually all sources, using several specific examples. Viii Deviations from the frequently used Eν−2 neutrino flux assumption; see, for example, 46 While many of these effects have been studied elsewhere in the literature, we mainly show examples generated with the NeuCosmA Neutrinos from Cosmic Accelerators software in this paper to present them in a self-consistent way.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
