Dr Horst Fichtner (Ruhr University Bochum)
In recent years one could witness tremendous progress regarding the physics of the transport of cosmic rays in the heliosphere. This progress derives from both theoretical advances and new measurements from the outer boundary region of the heliosphere. At the same time theory and observations give new constraints on the local interstellar cosmic ray spectra. The talk will address...
Dr Yulia Kartavykh (University of Würzburg / Ioffe Physical-Technical Institute)
The missions STEREO A/B with large separation distances, together with ACE, SOHO, and WIND near Earth, provide a unique opportunity to observe solar energetic particles (SEP) over a large range of solar longitudes and latitudes in the inner heliosphere. It is evident from these observations that temporal and directional characteristics of solar energetic particles strongly depend on the...
Prof. Vladimir Ptuskin
The problems of cosmic ray transport in the Galaxy are discussed. The discussion covers the diffusion model of cosmic ray propagation in the Galaxy, the fluctuations of cosmic ray intensity due to random nature of sources, the collective effects of relativistic particles in the interstellar medium, the nature of “hardening” and “knee” in cosmic ray spectrum and the transition to extragalactic...
33. A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays
Dr Antje Putze (Oskar Klein Laboratory Stockolm)
We implemented a Markov Chain Monte Carlo (MCMC) technique within the USINE propagation package to estimate the probability-density functions for cosmic-ray transport and source parameters within an 1D diffusion model. From the measurement of the B/C ratio and radioactive cosmic-ray clocks, we calculate their probability density functions, with a special emphasis on the halo size L of the...
32. The Long-Term Azimuthal Structure of the Galactic Cosmic Ray Distribution due to Anisotropic Diffusion
Mr Frederic Effenberg (Ruhr University Bochum)
In the description of Cosmic Ray transport following the well-known Parker Transport Equation, the spatial diffusion of energetic particles, in general, has to be treated by employing a tensorial quantity for the diffusion, i.e. using different diffusion strengths along and perpendicular to the magnetic field, respectively. This leads to results for the distribution function of these particles...
Dr Julien Lavalle (IFT-Madrid)