Speaker
Description
Galactic cosmic rays propagating in interstellar space interact with gas and radiation fields producing gamma ray and neutrino emissions of comparable intensity. These emissions result in diffuse fluxes of secondary particles reaching the Earth that encode information on the space distribution, energy spectra and mass composition of the parent CR's in the entire volume of the Galaxy, where direct detection is not possible.
Extending the measurements of the diffuse gamma ray flux to very high energy (>100 TeV) and detecting a neutrino flux above the atmospheric foreground is of great importance for our understanding of cosmic ray acceleration in Galactic sources and of the magnetic structure of the Milky Way. The study of this energy range is of particular importance because the CR particles that generate gamma rays and neutrinos are around the prominent spectral feature known as the ``knee''.
The absorption probability for gamma rays of energy > 100 TeV is large and distorts the energy and angular distributions of the diffuse flux, but taking into account these effects it is possible to obtain very valuable information also from observations in this energy range.
In this work we compare our predictions on the diffuse gamma ray and neutrino fluxes at high energy, developed under different hypothesis, with the existing data of neutrino telescopes and gamma ray detectors, including the new results by the Tibet AS array above 100 TeV, and discuss the potential of future observations.
Keywords
Galactic Gamma rays; Neutrinos; Diffuse emission
| Subcategory | Theoretical Results |
|---|
