Modeling of Ring Current Development During the Super Storm in November 2003

1. Modeling of Ring Current Development During the Super Storm in November 2003 Mei-Ching Fok1, Thomas E. Moore1, Dominique C. Delcourt2, Steven P. Slinker3 Joel A. Fedder4, Yusuke Ebihara5, and Samuel T. Jones6 1NASA Goddard Space Flight Center, USA 2CETP-CNRS-IPSL, Saint-Maur des Fosse, France 3Naval Research Laboratory, USA 4Leading Edge Technology, Inc., USA 5Nagoya University, Japan 6University of Texas in Arlington, USA ST03-A0010 August 3, 2007 2007 AOGS Meeting, Bangkok, Thailand

2. Outline • The super storm in November 2003 • Lyon-Fedder-Mobarry (LFM) global magnetospheric simulation of the Nov03 storm • Modeling the polar wind and auroral wind (O+) outflow from the ionosphere during the Nov03 storm • Modeling the ring current development during the Nov03 storm with solar, polar and auroral sources • Roles of convection, ionospheric outflow and acceleration in magnetotail on ring current development

3. November 2003 Storm Solar wind velocity • Solar wind velocity increased to ~750km/s. Solar wind density • Solar wind density was unusually high IMF Bz • IMF Bz decreased to -50 nT. • Negative IMF Bz lasted for ~ 12 hours. Dst • Dst reached -472 nT.

4. LFM Simulation of the November 2003 Storm

5. Ionospheric Outflow Driven by MHD Condition

6. Calculation of Density and Temperature from Test-Particle Trajectories

7. The Comprehensive Ring Current Model (CRCM) Boundary Condition Solar, Polar, Auroral Winds Ring Current Phase Space Density Charge Exchange Drift Losses LFM Magnetic Field Magnetospheric Electric Field Field Aligned Current Ionospheric Electric Field Ionospheric Conductivity Cross Polar Cap Potential Drop

8. Ring Current Formed by Solar Wind Ions

9. Ring Current Formed by Auroral O+ Ions

10. Simulated Plasmasphere Evolution

11. Plasmasphere Erosion During the Storm • • • plasmasphere erosion

12. Ring Current Energy Variations During Storm fast recovery • Significant amount of ionospheric particles are found in the ring current. • Decay of heavy ions from the ionosphere contributes to fast recovery

13. Balance Between Nightside Injection and Dayside Loss Nightside injections surpass dayside losses

14. Role of Tail Acceleration in Ring Current Buildup Acceleration in Tail Hot and Dense Plasma Sheet Intense Ring Current Without tail acceleration: CRCM run with quiet-time boundary conditions DE Tail acceleration Energy increase mainly due to convection DE

15. Summary • The global magnetospheric configuration and ring current development during the storm on 20-21 November 2003 are simulated using the combined tool: LFM + Delcourt-particle-code + CRCM • Particles from solar wind (H+), auroral wind (O+) and polar wind (H+) are included as sources of ring current ions. • Auroral wind and polar wind outflow characteristics are driven by instantaneous MHD conditions at the ionosphere. • Contribution of auroral O+ to the ring current is comparable or higher than that of the solar wind source. The fast decay of O+ contributes to fast storm recovery. • Nightside injections surpass drift loss at the dayside magnetopause. • Tail acceleration and strong convection contribute almost equally to the ring current buildup.

16. Future Work - Missing Piece Ring Current Ion Loss due to interaction with Electromagnetic Ion Cyclotron Waves