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THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE

CRISM- 2011 , Montpellier, 27 June – 1 July, 2011. THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE. Y.Kartavykh University of Würzburg (Germany), Ioffe Physical -Technical Institute ( Russia ).

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THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE

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  1. CRISM-2011, Montpellier, 27 June – 1 July, 2011 THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE Y.Kartavykh University of Würzburg (Germany), IoffePhysical-Technical Institute (Russia) Collaborators: W. Dröge, B. Klecker, G.A. Kovaltsov

  2. Solar cosmic rays = Solar Energetic Particles • Generated in solar explosive processes • Short time scale in comparison with time scales typical for GCR • Anisotropic fluxes at ~ 1 AU

  3. gamma-rayimagingof solar flares reconstructionofeventgeometry aretheremorethanoneacceleration processes, stages, phases? areinteractingandescapingparticles fromthe same population?

  4. energetic particles in the Heliosphere focus here on particles from impulsive events avoids complications due to CMEs and interplanetary shocks realistic transport models required to reconstruct particle properties at the Sun from spacecraft observations: acceleration time scales, energy and charge spectra, relation to electromagnetic emission close to the Sun (radio, X-ray, gamma-ray)

  5. Because of anisotropy in SEP events one should consider pitch-angle diffusion 5 Dec 1997 107 keV electrons Wind 3DP PI: R.P.Lin Pitch-angle distributions for the 2003, March, 17 event

  6. Early Multi-SpacecraftObservationsof Impulsive Solar Events Wibberenz & Cane (2006) electrons in the MeV range can be detected more than 80 degreesfrom the flare longitude evidence for lateral transport Connection plot and electrontime profiles for theflare event of 1979January 15. Variation of peak intensitiesIm with connection angle

  7. DROPOUTS CUTOFFS STEPS Mazur et al. (2000) ACE ULEIS 1 May 2000 Wind 3DP 4 Nov 1997 • no velocitiy dispersion • time variations correspond to spatial gradients perpendicular • to B which are convected past the spacecraft goal: find a suitable phenomenological description which can be used as starting point for comparison with theory

  8. SOLAR PARTICLE PROPAGATION COMBINATION OF: AZIMUTHAL TRANSPORT CLOSE TO THE SUN (CORONAL DIFFUSION) TRANSPORT PARALLEL TO B PITCH ANGLE SCATTERING, FOCUSING, ADIABATIC LOSSES POSSIBLE DIFFUSION ACROSS THE AVERAGE MAGNETIC FIELD considered here only particles from impulsive events avoids complications due to CMEs and shocks

  9. In our model we solve stochastic differential equations Resultsofthe model: - SEP‘ time profiles - spatialdistributions - pitch-angle distributions (therefore, anisotropy, too)

  10. Parker field

  11. Droege et al, 2010 Way of 4 MeV proton, with and without perpendicular diffusion. =0.01 , =0.3 / cos AU cos=1/(1+2sin2r2/Usw2)0.5

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

  13. 107 keV electrons 0.75-1.25 h Droege et al, 2010

  14. Protons, 4 MeV, 23.5-24.5 hrs Droege et al, 2010

  15. Droege et al, 2010

  16. No perpdiff, one-dimensional or homogen. Perpdiff, no corotation Corotation, no perpdiff, perpdiff, 4 degr. flank Droege et al, 2010

  17. Electronintensities in theenergyrange 65-105 keVat 1 AU, withoutperpendiculardiffusion, andfortwovaluesofα. Angular distancesof SC tothesourcearegiven on thelegends.

  18. Anisotropiesofelectrons. Upperpanel: locationof SC on themagneticlineconnectedtotheflare, α=0.01. Middlepanel: angle ofobservations 30 degrees, α=0.01. Lowerpanel: angle ofobservations 30 degrees, α=0.1. In all cases

  19. Comparisonofprotonsintensities, observedfrom different longitudes, at a radial distance 0.31 AU (see legend) in caseof multiple injectionfromthepoint-likesource. Comparisonofprotonsintensities, observedfrom different longitudes, at a radial distance 1 AU (see legend) in caseof multiple injectionfromthepoint-likesource.

  20. 2010, January 17 event From N.Dresing

  21. 2010, August, 18 event From R.Gόmes-Herrero

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

  23. 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.

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