Erlangen 2026 – scientific programme
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T: Fachverband Teilchenphysik
T 62: Cosmic Rays III
T 62.6: Talk
Wednesday, March 18, 2026, 17:30–17:45, KS 00.006
Revised Diffusive Shock Acceleration with CRPropa3.2 for the description of cosmic ray spectra at supernova shocks — •Jakob Dörner1, Sophie Aerdker1,2, Lukas Merten1,2, and Julia Tjus1,2,3 — 1Theoretical Physics IV: Plasma-Astroparticle Physics, Faculty for Physics & Astronomy, Ruhr University Bochum, Germany; Supported by SFB1491 — 2Ruhr Astroparticle and Plasma Physics Center (RAPP Center) — 3Department of Space, Earth and Environment, Chalmers University of Technology, Gothenburg, Sweden
Supernova remnants (SNRs) play an important role in the acceleration of Galactic cosmic rays (CRs) that gain significant energy by repeatedly crossing the shock front. This acceleration process, known as diffusive shock acceleration (DSA), generally leads to a power-law spectral slope of E−2. However, observations of nonthermal emission of SNRs imply CR energy distributions that are generally softer than E−2, the DSA prediction. In contrast, non-linear theory of DSA would predict an even harder spectrum. Recent studies suggest that such soft spectra may arise from the additional drift of magnetic structures with respect to the thermal plasma downstream of the shock. We incorporate the effect of such drifts by changing the effective compression ratio of the shock in test particle simulations using the CRPropa framework, which solves the transport equation by utilizing stochastic differential equations. We obtain soft energy spectra, depending on the strength of the effective compression ratio, and concave energy spectra when the precursor is taken into account.
Keywords: Acceleration of Particles; Supernova Remnants; Stochastic Differential Equations