ULF Wave Modelling With A Motive: Effects on Energetic Paritcles

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

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 CRRES 18 degree inclination, 6.3 RE apogee, July 90 – Oct 91 Hudson et al., Annales. Geophys., 2004

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

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 δv ~ δE/B_0 Proehl et al., JGR 2002

14. Parallel Mode Structure Poloidal mL=1/3

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

16. Goodrich et al. ‘98

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

18. Azimuthal Distribution of P(Ephi)

19. Azimuthal Distribution of P(Ephi)

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

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 • 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: 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 ~ LN Falthammar, 1965 N=6, 10Elkington et al., 2003N=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 Storm Fei et al., 2005

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

34. EF 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 by inductive EF 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 March 24, 91 event Hudson et al., JGR, 1997

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 • 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 1st invariant conserved (Young et al., 2002)

44. Higher Frequency Wave Mode Effects • Other, 1st 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 Sharper dawn-side radial gradient affects ionospheric screening (Glassmeir & Stellmacher, JGR, 2000) Duskside B-compression affects K-H instability threshold velocity shear (Lee et al., JGR, 1981)

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