GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions

Abstract

Recent discoveries in astrophysics of cosmic rays (CR) and γ-ray astronomy demand more accurate and reliable CR propagation code. Having 21 years of development behind it, the GALPROP model has become a de-facto standard in astrophysics of CR, diffuse γ-rays, and searches of new physics. The GALPROP project is devoted to the development of a self-consistent model for CR propagation in the Galaxy and associated diffuse emissions (radio, microwave, X-rays, γ-rays). The project stimulated independent studies of the interstellar radiation field (ISRF), distribution of the interstellar gas (H 2 , H I, H II), synchrotron emission and the Galactic magnetic field, and a new study of the isotopic production cross sections. These studies provide necessary and unique input datasets for the GALPROP model. The code is optimized and parallelized and accessible as a standalone executable or library that can be linked to other codes enabling many other studies, such as Markov Chain Monte Carlo, MultiNest, SuperBayeS, and DarkSUSY. The new version of the code has many updates that improve its accuracy and capabilities. As always, the latest release of the code is available through the WebRun, a service to the scientific community enabling easy use of the GALPROP code via web browsers.35th International Cosmic Ray Conference

HelMod in the Works: From Direct Observations to the Local Interstellar Spectrum of Cosmic-Ray Electrons

“…GALPROP includes a description for the processes of K-capture, electron capture by bare CR nuclei and stripping, as well as knock-on electrons. More details are given in Ptuskin et al (2006), Strong et al (2007), Vladimirov et al (2011), andJóhannesson et al (2016), as well as the description of the most recent version of GALPROP (v. 56; see Moskalenko et al (2017) and Porter et al (2017), and references therein).…”

Dark matter phenomena

“…IceCube: Search for neutrinos from dark matter annihilations in the Sun M. Rameez Figure 5: Limits on the spin dependent WIMP-Nucleon scattering cross section as a function of the WIMP mass, derived from this analysis and compared to other experiments' limits from [15,18,19,21,22]. The red band around the limit signifies systematic uncertainties.…”

“…While diffusing, charged CRs experience several other processes, and in particular energy losses due to synchrotron radiation, Inverse Compton Scattering (ICS) on the low energy photons of the CMB and starlight, Coulomb losses, bremsstrahlung, nuclear spallations... . The transport process is solved numerically or semianalytically using codes such as GALPROP [22], DRAGON [23], USINE [24], PICARD [25].…”

The Interstellar Radiation Field of the Milky Way in Three Spatial Dimensions

“…The direct application to interpreting high-energy γ-ray data with 3D CR source and ISRF spatial density models will be described at the meeting [29]. The data files for both 3D ISRF models will be made available from the GALPROP website and can be used with the forthcoming release of the GALPROP code [30].…”