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.Drge (1), G.Kovaltsov (2), R.Gomes-Herrero (3), N.Dresing (3), B.Klecker (4), B.Heber (3) (1) University of Wrzburg, Germany (2) Ioffe Physical-Technical Institute, Russia (3) Christian-Albrechts-Universitt Kiel, Germany (4) Max-Planck-Institut fr extraterrestrische Physik, Garching, Germany 2010, January 17 event From N.Dresing 2 : 3 From N.Dresing 2010, August, 18 event From R.Gmes-Herrero See poster : , additional separat. by 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) Parker field 6 Protons, 4 MeV hrs 7 Droege et al, 2010 8 9 10 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) 107 keV electrons h 12 Droege et al, 2010 Electron intensities in the energy range keV at 1 AU, without perpendicular diffusion, and for two values of . Angular distances of SC to the source are given on the legends. 13 Different angles of observation, values of are given on the legend Anisotropies of electrons. Upper panel: location of SC on the magnetic line connected to the flare, =0.01. Middle panel: angle of observations 30 degrees, =0.01. Lower panel: angle of observations 30 degrees, =0.1. In all cases 14 =0, =0.01 =30, =0.01 =30, =0.1 15 R SC = 1.0 AU, different values of rmfp ( r ) are given on the legend 16 Different values of are given on the legends 17 R SC = 0.3 AU R SC = 1.0 AU 18 Asymmetry observation from east west relative to the source 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 20 21 Time profiles from point-like source August, 2010 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