Results 251 to 260 of about 228,178 (278)
Some of the next articles are maybe not open access.
2010
Once accelerated at supernova shocks, cosmic rays have to propagate through the interstellar medium before we detect them. The interstellar medium contains matter, magnetic fields and radiation fields, all of which are targets for cosmic ray interactions. Cosmic ray protons scatter in the magnetic fields and slowly diffuse away from their sources.
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Once accelerated at supernova shocks, cosmic rays have to propagate through the interstellar medium before we detect them. The interstellar medium contains matter, magnetic fields and radiation fields, all of which are targets for cosmic ray interactions. Cosmic ray protons scatter in the magnetic fields and slowly diffuse away from their sources.
openaire +1 more source
2010
As we discussed in the previous chapter, primary cosmic rays interact with the atmosphere and produce fluxes of secondary, tertiary, etc. particles. All these particles together create a cascade, called an air shower. In principle, measurements of air shower particles can be interpreted in terms of the energy spectrum and the composition of the primary
openaire +1 more source
As we discussed in the previous chapter, primary cosmic rays interact with the atmosphere and produce fluxes of secondary, tertiary, etc. particles. All these particles together create a cascade, called an air shower. In principle, measurements of air shower particles can be interpreted in terms of the energy spectrum and the composition of the primary
openaire +1 more source
Applications of cosmic-ray muons
Progress in Particle and Nuclear Physics, 2020G Bonomi, P Checchia, M D'Errico
exaly
Self-generated cosmic-ray turbulence can explain the morphology of TeV halos
Physical Review D, 2022Payel Mukhopadhyay, Tim Linden
exaly