Transport of cosmic rays from supernova remnants through the galactic magnetic field

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Supernova remnants (SNRs) are the primary candidates for the explanation of the cosmic ray flux up to 1015 eV. In this project, cosmic ray transport will be simulated, including discrete SNRs with individually modeled spectra. The simulated leptonic and hadronic cosmic ray spectra after propagation will be compared with the observed spectra. In particular, the inclusion of discrete sources and convection in the transport simulation is expected to contribute further to the explanation of some of the observed anomalies, like the hadronic cosmic ray anisotropy at 10 TeV, high-energy electron and positron spectra, and the haze photon structure from towards the Galactic center