- Conference date: 17-31 June 2002
- Location: Pisa (Italy)
In order to interpret the fluxes of particles accelerated at corotating interaction regions and to forecast the solar energetic particle events, the propagation of energetic particles is investigated numerically. Particle transport is influenced in a strong way by the magnetohydrodynamic turbulence in the solar wind. We carried out a simulation in which ions are injected in a numerical realization of magnetic turbulence superimposed on a background uniform magnetic field. Particle transport is studied as a function of particle energy, pitch angle distribution, turbulence level, and turbulence anisotropy with parameter values appropriate to the solar wind. The ratio of perpendicular to parallel diffusion coefficients is estimated. For strong enough turbulence δB/B 0 ∼ 1, as typical of the solar wind, we find that the particle pitch‐angle distribution is quickly isotropized, and that perpendicular transport grows with the particle energy. Varying the turbulence anisotropy, that is the turbulence correlation lengths l ∥ and l ⊥, we find that in the cases with l ∥ ≫ l ⊥ (i.e., in the limit of 2D turbulence) the particle perpendicular transport is faster than in the cases with l ∥ ≪ l ⊥ (i.e., for the so called slab turbulence).
- Turbulent flows
- Turbulent transport processes
- Solar wind
- Solar energy
- Wind energy
Y. K. Semertzidis, M. Aoki, M. Auzinsh, V. Balakin, A. Bazhan, G. W. Bennett, R. M. Carey, P. Cushman, P. T. Debevec, A. Dudnikov, F. J. M. Farley, D. W. Hertzog, M. Iwasaki, K. Jungmann, D. Kawall, B. Khazin, I. B. Khriplovich, B. Kirk, Y. Kuno, D. M. Lazarus, L. B. Leipuner, V. Logashenko, K. R. Lynch, W. J. Marciano, R. McNabb, W. Meng, J. P. Miller, W. M. Morse, C. J. G. Onderwater, Y. F. Orlov, C. S. Ozben, R. Prigl, S. Rescia, B. L. Roberts, N. Shafer‐Ray, A. Silenko, E. J. Stephenson, K. Yoshimura and EDM Collaboration
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