12-20 July 2017
Asia/Seoul timezone
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BEXCO - Room F(201/202/203/204)

[CRI098] DRAGON2: new features on energy losses treatment


  • Arianna LIGORINI

Primary authors


  • Carmelo EVOLI (Gran Sasso Science Institute, Italy)
  • Daniele GAGGERO (GRAPPA Institute, University of Amsterdam, The Netherlands)
  • Andrea VITTINO (Physik-Department T30d, Technische Universitat Munchen, Germany)
  • Giuseppe Di BERNARDO (Max-Planck-Institut fur Astrophysik, Garching bei Munchen, Germany)
  • Mattia Di MAURO (W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics)
  • Dario GRASSO (INFN and Dipartimento di Fisica “E. Fermi”, Pisa University, Italy)
  • Piero ULLIO (Scuola Internazionale di Studi Superiori Avanzati, Italy)


In recent years we witnessed several experiments measuring a large set of observables related to Cosmic-ray physics with an unprecedented level of precision. In order to be able to fully exploit this great amount of new data we must act to refine our theoretical predictions. This can be achieved by building more realistic models of Cosmic-ray Galactic transport. The DRAGON project has been pursued in order to model Cosmic-rays propagation under realistic conditions and to allow a comparison with a wide set of experimental data. Studies brought forth with DRAGON showed how a treatment of Cosmic rays energy losses as realistic as possible is pivotal. In DRAGON2, the new version of the code, a more accurate, second order scheme for Cosmic Rays energy losses is implemented. In addition, the new version of the code allows us to investigate the impact of different models for Interstellar Radiation Field or galactic magnetic field. We present comparison between the previous energy losses approach and the new one, as well as validation test by comparing our numerical results with a set of analytical solutions. We study in particular the interplay of diffusion, reacceleration, and energy losses in a realistic case, and their impact on leptonic spectrum.