Cosmic-ray propagation and interactions in the Galaxy
read the original abstract
We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy up to energies of 10^15 eV. A guide to the previous reviews and essential literature is given, followed by an exposition of basic principles. The basic ideas of cosmic-ray propagation are described, and the physical origin of its processes are explained. The various techniques for computing the observational consequences of the theory are described and contrasted. These include analytical and numerical techniques. We present the comparison of models with data including direct and indirect - especially gamma-ray - observations, and indicate what we can learn about cosmic-ray propagation. Some particular important topics including electrons and antiparticles are chosen for discussion.
This paper has not been read by Pith yet.
Forward citations
Cited by 5 Pith papers
-
Charge-dependent spectral softenings of primary cosmic-rays below the knee
Direct measurements reveal charge-dependent spectral softenings in primary cosmic rays at a common rigidity of ~15 TV, rejecting mass-dependent softening at >99.999% confidence.
-
On the contribution of the bow shock pulsar wind nebula PSR J0437-4715 to the observed fluxes of GeV-TeV positrons and antiprotons
The bow shock pulsar wind nebula around PSR J0437-4715 explains the GeV-TeV positron excess and hundreds-of-GeV antiproton flux with an energy-independent ratio by using 25% of the pulsar's wind power.
-
Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions
Galactic synchrotron emissions above 20 MHz can set tighter upper limits on the abundance of primordial black holes with masses above 10^16 grams than previous cosmic-ray electron data.
-
Proton-Proton to Antinucleon Cross Sections for Cosmic Ray Applications
NLO perturbative QCD calculations predict only a mild few-percent excess of antineutrons over antiprotons in pp collisions, not supporting the ~30% excess reported by NA49.
-
On The Nonthermal Power Laws In Magnetized Turbulent Plasmas
A scaling law for nonthermal power-law tails in magnetized turbulent plasmas is derived from particle transport principles and confirmed by PIC simulations with escape, with applications to black hole coronae.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.