1. Multi-Fluid/Particle Treatment of Magnetospheric- Ionospheric Coupling During Substorms and Storms R. M. Winglee

2.  Strong Heavy Ion Ionospheric Outflows observed during active periods  Substantial Asymmetries that provide key insight during active periods  Multi-Fluid Equations ideal substorm Particle acceleration associated with boundary layers Magnetic reconnection & current sheet acceleration Influence of heavy ions on the global dynamics  Application to the Storm of April 17, 2003

3. Yau and Andre, 1997

4. Speiser, 1965

5. Iijima and Potemra, 1978 Dawn-Dusk Merging of Field- Aligned Currents Systems R1 R2

6. Ogino, 1986 Ideal MHD Current: Anti-symmetric

7. Multi-Fluid Equations Ideal MHD Neglect all cyclotron terms No Current Sheet Acceleration (aka Speiser motion) No Parallel Electric Fields No Ion Differentiation Accurate treat of system if its is in pressure balance

8. Multi-Fluid Equations More Accurate Solution

9. For the Ions Not Zero

10. Inner Radius : 2.5 R e Grid Resolution: 0.25 R e Fixed Ionospheric Density and Temperature; Zero Velocity Resistive Earth/Atmos. , T, V determine by magnetospheric driving and ionospheric conditions Gravity Polar (Thermal) Winds H + : 400 cm -3, 10 eV eq., 0.1 eV polar O + : 5%

11. Zero IMF Southward IMF (-8 nT for 80 min) Northward IMF (8 nT for 60 min)

12. T = 0250 T = 0313 T = 0430 12 00 1806 T = 0337 12 00 1806 T = 0420 T = 0410

15. Solar Wind Density 1 0.01 cm -3 -50 R e 20 R e

16. Ionospheric H + Density 1 0.01 cm -3 -50 R e 20 R e

17. Relative Ionospheric O + Density 40 20 % 10 -50 R e 20 R e

18. Ionospheric O + Temperature -50 R e 20 R e

19. Cross-Polar Cap Potential

20. Effective Plasma Resistivity (Cross-Polar Cap Potential/Total Ionospheric Current)

21. Effective Ohmic Dissipation (Cross-Polar Cap Potential*Total Ionospheric Current)

22. Modification of reconnection Side View -50 R e 20 R e

23. Modification of reconnection Top View -50 R e 20 R e

24. Midnight O + Ionospheric Outflow 50 Re 20 Re Dusk Dawn Velocity (1000 km/s)

25. Midnight O + Ionospheric Outflow 12 00 18 06

26. Full O + Ionospheric Outflow 12 00 18 06

27.  Larger response of heavy ionospheric ions to activity and increases the effective ionospheric conductivity  Midnight light ions and pre-midnight heavy ions have access to tail reconnection region  Acceleration leads to locally high concentrations of O + AND asymmetric tail reconnection  Ion cyclotron affects lead to the generation of flux ropes  The asymmetries lead to distortion of the field-aligned current system M/I Coupling for an Idealized Substorm

28. Apr 17, 2002 Storm

32. Solar Wind Density

33. Relative O + Density

34. Ionospheric H + Temperature

35. Equatorial B z Positive Negative

36. Top View of Magnetic Field lines

37. Storm Activity  Northward pressure pulse leads to large entry of solar wind plasma  Eventually excluded by ionospheric plasma  Large IMF swings allow protons not oxygen to rapidly respond  Both increases and decreases in effective conductivity  Large IMF variations also allow both sunward and tailward motion of the near-Earth neutral line  Latter part of the even during sustained southward IMF should allow build up of O +

38. Ionospheric O + Density 1 0.01 cm -3

39. Solar Wind Temperature

40. Ionospheric H + Temperature

41. Duskside O + Ionospheric Outflow Velocity (1000 km/s) 55 Re 16 Re Dusk Dawn

42. Duskside O + Ionospheric Outflow 12 00 18 06

43. Cusp O + Ionospheric Outflow Velocity (1000 km/s) 55 Re 16 Re Dusk Dawn

44. Cusp O + Ionospheric Outflow 12 00 18 06

45. Dawn O + Ionospheric Outflow 55 Re 16 Re Dusk Dawn Velocity (1000 km/s)

46. Dawn O + Ionospheric Outflow 12 00 18 06