1. THREE-DIMENSIONAL ANISOTROPIC TRANSPORT SIMULATIONS: A PARAMETER STUDY FOR THE INTERPRETATION OF MULTI-SPACECRAFT SOLAR ENERGETIC PARTICLE OBSERVATIONS 32-nd International Cosmic Ray Conference August 11 – 18, 2011, Beijing, China 1 Y.Kartavykh (1,2), W.Dröge (1), G.Kovaltsov (2), R.Gomes-Herrero (3), N.Dresing (3), B.Klecker (4), B.Heber (3) (1) University of Würzburg, Germany (2) Ioffe Physical-Technical Institute, Russia (3) Christian-Albrechts-Universität Kiel, Germany (4) Max-Planck-Institut für extraterrestrische Physik, Garching, Germany

2. 2010, January 17 event From N.Dresing 2 Δφ : -108 -169 118

3. 3 From N.Dresing

4. 2010, August, 18 event From R.Gόmes-Herrero See poster 0947 4 Δφ: 91 35 -43, additional separat. by θ

5. In our model we solve stochastic differential equations by time-forward M.-C. method 5 Results of the model: - SEP‘ time profiles - spatial distributions - pitch-angle distributions (therefore, anisotropies, too)

6. Parker field 6

7. Protons, 4 MeV 3.5-4.5 hrs 7 Droege et al, 2010

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11. Rsc =0.31 AU, SC is at 15 degress to the east (-15 degrees) SC at the connecting mfl (0 degress) SC is at 15 degrees to the west (+15 degrees) 11 protons Rsc =1 AU, SC is at 15 degress to the east (-15 degrees) SC at the connecting mfl (0 degress) SC is at 15 degrees to the west (+15 degrees)

12. 107 keV electrons 0.75-1.25 h 12 Droege et al, 2010

13. Electron intensities in the energy range 65-105 keV at 1 AU, without perpendicular diffusion, and for two values of α. Angular distances of SC to the source are given on the legends. 13 Different angles of observation, values of Δφ are given on the legend

14. Anisotropies of electrons. Upper panel: location of SC on the magnetic line connected to the flare, α=0.01. Middle panel: angle of observations 30 degrees, α=0.01. Lower panel: angle of observations 30 degrees, α=0.1. In all cases 14 Δφ=0, α=0.01 Δφ=30, α=0.01 Δφ=30, α=0.1

15. 15 R SC = 1.0 AU, different values of rmfp ( λ r ) are given on the legend

16. 16 Different values of α are given on the legends

17. 17 R SC = 0.3 AU R SC = 1.0 AU

18. 18 Asymmetry – observation from east – west relative to the source

19. C O N C L U S I O N S - Propagation of charged particles in a magnetic field strong in comparison with superposed irregularities should be considered in a pitch-angle diffusion approximation - The observed sharp intensities variations (cutoffs and drop-outs) can be explained by a very weak diffusion in a perpendicular to the large scale magnetic filed direction - The existing multispacecraft observations can serve as a tool to determine the characteristics of interplanetary space - Time profiles, together with directional properties of SEP events strongly depend on the angular distance and distance along the magnetic field line from the source. 19

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22. Time profiles from point-like source 22 18 August, 2010

23. Magenta curve – no adiabatic losses, no perp. diff Black – no perp diff., but adiabatic losses Green – no adiabatic losses, but perp. diff. Red – both, adiabatic losses and perp. diff. 23