1. ULF Wave Modelling With A Motive: Effects on Energetic Paritcles Mary Hudson, Scot Elkington, Brian Kress, Kara Perry, John Lyon, Mike Wiltberger

2. ULF Wave-Relativistic Electron Correlation Rostoker et al., GRL, 1998

3. Toroidal and Polodial Modes Hughes, Solar Wind Sources of Magnetospheric ULF Waves, AGU, 1994

4. CRRES Poloidal and Toriodal ULF Wave B Components Hudson et al., Annales. Geophys., 2004 CRRES 18 degree inclination, 6.3 RE apogee, July 90 – Oct 91

5. CRRES Occurrence Rates of Poloidal and Toroidal ULF Waves Hudson et al., Annales Geophys., 2004

6. AMPTE CCE Occurrence Rates Of Toroidal Mode 9 RE apogee Takahashi et al., JGR, 2002

7. AMPTE IRM Occurrence Rates Of Poloidal/Compressional Mode Anderson et al., JGR 1990

8. Mathie & Mann JGR 2000 Mathie & Mann 2000 JGR Groundbased Magnetometer ULF Wave Studies

9. Pc5 Correlation with Solar Wind Speed and Relativistic Electrons Mann et al., JASTP, 2004

10. Convective Growth of Magnetopause K-H Waves Miura, JGR, 1992

11. Direct Coupling of Solar Wind ULF Waves Kepko et al., GRL, 2002

12. Transmitting ULF Wave Power Into Magnetosphere via Fast Mode

13. Structure of Externally Driven FLRs Linear dipole MHD simulation Proehl et al., JGR 2002 δv ~ δE/B_0

14. Parallel Mode Structure Poloidal m L = 1/3

15. Global LFM-MHD Simulations of Magnetosphere Solar wind measurements made by satellite at L1, or CME-solar wind coupled MHD codes Solar wind measurements made by satellite at L1, or CME-solar wind coupled MHD codes Ideal MHD equations are solved on a computational grid to simulate the response of the magnetosphere Ideal MHD equations are solved on a computational grid to simulate the response of the magnetosphere

16. Goodrich et al. ‘98

17. L dependence of Ephi power Elkington, S. R., M. Wiltberger, A. A. Chan, and D. N. Baker, J. Atmos. Solar Terr. Phys., 66, 1371, 2004. 0.558-15 mHz

18. Azimuthal Distribution of P(Ephi)

20. Azimuthal Mode Number from MHD Simulations and Ground Magnetometers Mathie & Mann, JGR, 2000 Sept 98 storm MHD (Ephi) wave power in 0.14-15 mHz, low m modes

21. Frequency Dependence Bloom, R. M. and H. J. Singer, JGR, 100, 14943, 1995.

22. Convective Growth of Magnetopause K-H Waves

24. K-H Shear-Driven Instability

25. Direct Coupling of Solar Wind ULF Waves Kepko et al., GRL, 2002

26. 3 MHz Solar Wind Pulsations

27. SW Density Driven Pulsations

28. Test Particle Simulations of Radiation Belts 2D: Drift motion of electrons and ions in the equatorial plane is followed using time- varying electric and magnetic fields from global MHD simulation 2D: Drift motion of electrons and ions in the equatorial plane is followed using time- varying electric and magnetic fields from global MHD simulation 3D: Bounce and drift motion of guiding center electrons in MHD fields; gyro, bounce and drift motion of Solar Energetic Particles (el, protons, Fe) 3D: Bounce and drift motion of guiding center electrons in MHD fields; gyro, bounce and drift motion of Solar Energetic Particles (el, protons, Fe) Solar Energetic Particle (SEP) cutoffs calculated using MHD fields

29. MHD Fields Injection of RadBelt Electrons

30. Radiation Belt Electron Energization Processes Conserving First Invariant Particles can be energized by: Particles can be energized by: 1)Convection: steady, or substorm and storm-enhanced 1)Convection: steady, or substorm and storm-enhanced 2)Diffusion*: convection E fluctuations, ULF wave δE and δB  δE enhance diffusion 3) Drift time scale injection (Mar 91) a)Falthammar, JGR, 1965; b)Elkington et al., JGR, 2003 *

31. Diffusion Rates vs. L Radial diffusion rates in model ULF wave fields D_LL ~ L N Falthammar, 1965 N=6, 10 Elkington et al., 2003 N=11 Selesnick et al., 97, 2000 N=12 Perry et al., JGR, 2005, N=6, 18 Perry includes δEφ, δBr, δB//, freq and L-dependent Power Braughtigam & Albert, 2000, N=6, 10

32. MHD-Driven Phase Space Density AE8 Max-Initialized, Sept 98 StormFei et al., 2005

33. Drift Time Scale Injection from SSC’s Drift Time Scale Injection from SSC’s Blake et al., 2005

34. E  in equatorial plane from MHD simulation of March 24, 1991 CME-interplanetary shock compression of magnetopause. E x B transport of ring of radiation belt electrons inward E x B transport of ring of radiation belt electrons inward by inductive E  due to magnetopause compression dBz/dt. by inductive E  due to magnetopause compression dBz/dt.

35. MHD-Guiding Center Simulation Elkington et al., JASTP, 2002; 2004

36. Equatorial Plane Proton MHD Guiding Center Simulation Hudson et al., JGR, 1997March 24, 91 event

37. Average Count Rate of 10-20 MeV Electrons Mirroring at SAMPEX

38. Solar Proton Trapping Nov 01

39. New belt example: 24 Nov 2001 Clear trapping of solar particles - no other source of heavy ions possible Mazur et al., SHINE mtg, 2004

40. Solar Energetic Particle Access

43. Summary of ‘ULF Wave’ Effects on Energetic Particles Electrons interact diffusively with ULF waves with f ~ electron drift period while conserving first invariant Electrons interact diffusively with ULF waves with f ~ electron drift period while conserving first invariant Large amplitude distortion of magnetopause launches magnetosonic impulse outside range of linear ULF wave models, drift time scale injection of MeV electrons and protons (electrons unusual) Large amplitude distortion of magnetopause launches magnetosonic impulse outside range of linear ULF wave models, drift time scale injection of MeV electrons and protons (electrons unusual) Solar energetic particles trapped on drift time scale, stay trapped as long as 1 st invariant conserved (Young et al., 2002) Solar energetic particles trapped on drift time scale, stay trapped as long as 1 st invariant conserved (Young et al., 2002)

44. Higher Frequency Wave Mode Effects Other, 1 st invariant violating processes responsible for energy/momentum diffusion and pitch angle diffusion at fixed L (VLF/ELF) Other, 1 st invariant violating processes responsible for energy/momentum diffusion and pitch angle diffusion at fixed L (VLF/ELF) Summers and Ma, JGR, 2000

45. Externally and Internally Excited Pc5 (mHz) ULF Waves: low and high m

46. Field Line Resonance

47. Dawn-Dusk Assymmetry in Toroidal Mode ULF Wave Power Duskside B-compression affects K-H instability threshold velocity shear (Lee et al., JGR, 1981) Sharper dawn-side radial gradient affects ionospheric screening (Glassmeir & Stellmacher, JGR, 2000)

48. Compressed (solid) vs. dipole (dashed) diffusion coefficients Perry et al., JGR, 2005