Cosmic-Ray Propagation and Interactions in the Galaxy

By A. Strong, Igor V. Moskalenko, V. Ptuskin. 2007

970 citations recorded by the source corpus.

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 is 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 γ-ray—observations, and indicate what we can learn about cosmic-ray propagation. Some important topics, including electron and antiparticle propagation, are chosen for discussion.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1aaa87a44433d94e4e2da6640ee25681f1808dee

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Citations in the corpus

FERMI OBSERVATIONS OF CASSIOPEIA AND CEPHEUS: DIFFUSE GAMMA-RAY EMISSION IN THE OUTER GALAXY (2009, result): “We further compare our results with the predictions by GALPROP, a physical model of CR propagation in the Galaxy (see e.g. Strong & Moskalenko 1998; Strong et al. 2004a, 2007).”
A database of charged cosmic rays (2013, methodology): “The CR data are the backbone of Galactic CR propagation studies (e.g., Jones et al. 2001; Maurin et al. 2001; Strong et al. 2007; Evoli et al. 2008).”
Pulsars versus dark matter interpretation of ATIC/PAMELA (2009, methodology): “In the energy range 10 GeV – 1 TeV, these backgrounds agree with [36] and with the gamma-ray and synchrotron studies [21].”
Background model systematics for the Fermi GeV excess (2014, methodology): “1 Building GDE models with Galprop In our analysis, we make use of the Galprop v54 code [106–108] to produce gamma-ray templates for the GDE at various energies.”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “The corresponding emission processes are modelled in detail in e.g. the GALPROP code (Strong et al., 2007), which includes 3D distributions of interstellar gas and photon fields, as well as all relevant interaction cross sections and constraints from near-Earth observations of cosmic-ray fluxes and…”
SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS (2010, background): “…characteristics of cosmic ray propagation in the Galaxy needed for calculation of the cosmic ray spectrum in the so called leaky-box approximation is the escape length Xe, that is the average matter thickness traversed by cosmic rays before they exit from the Galaxy, see e.g. Strong et al. (2007).”
A NEW MODEL OF THE GALACTIC MAGNETIC FIELD (2012, methodology): “To investigate further the degeneracy between striated fields and the relativistic electron density (and the sensitivity of our best-fit magnetic field parameters to the uncertainty in ncre) we made the following test: we reoptimize the field parameters after multiplying the GALPROP ncre by a factor”
THE FERMI BUBBLES. I. POSSIBLE EVIDENCE FOR RECENT AGN JET ACTIVITY IN THE GALAXY (2011, neutral): “Typical values of κ for 1 GeV CRs are found to be κ ∼ (3 − 5) × 1028 cm2 s−1 in the solar vicinity (Strong et al. 2007).”
Inverse Compton Origin of the Hard X-Ray and Soft Gamma-Ray Emission from the Galactic Ridge (2008, background): “For recent reviews see Moskalenko et al. (2004), Strong et al. (2007), and references therein.”
A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays - II. Results for the diffusion model combining B/C and radioactive nuclei (2010, background): “The set of j = 1 . . . n equations governing the propagation of n CR nuclei in the Galaxy is described in Berezinskii et al. (1990).”
The Fermi Galactic Center GeV Excess and Implications for Dark Matter (2017, methodology): “…we will model Galactic interstellar emission from the large-scale CR populations in the Galaxy starting from predictions obtained through the GALPROP code71 (Moskalenko & Strong 1998; Strong et al. 2000, 2004; Ptuskin et al. 2006; Strong et al. 2007; Porter et al. 2008; Vladimirov et al. 2011).”
GLOBAL COSMIC-RAY-RELATED LUMINOSITY AND ENERGY BUDGET OF THE MILKY WAY (2010, methodology): “…with the diffusive reaccelation characterised byan Alfvén speed,vA, assuming a Kolmogorov spectrum of interstellar turbulence (if used), and the size of the CR confinement volume,zh, are obtained by fitting the CR secondary/primary ratios for B/C and10Be/9Be; for details see Strong et al. (2007).”