Moore Plasma Circulation ESSE06

Magnetospheric Plasma Circulation: 

Magnetospheric Plasma Circulation T E Moore1, M-C Fok1, D C Delcourt2, S Slinker3, J Fedder4, M Buenfil1 NASA’s Goddard Space Flight Center CETP, St.-Maur, France Naval Research Laboratory LET Corp. Moore, Fok, et al., JGR Feb 2005 “Solar and Polar Wind…” Moore, Fok, et al., Geophys. Mono. 159, 2005, “Ionospheric Plasmas in the Ring Current” Nosé, Christon, Taguchi, Moore, Collier, JGR 2005, “Overwhelming O+… Inferred ablation of Osiris’ atmosphere

Halloween 2003 on DST Trend: 

Halloween 2003 on DST Trend Nosé, Christon, Taguchi, Moore, Collier, JGR 2005, “Overwhelming O+…

Halloween Outflows TIDE and LENA: 

Halloween Outflows TIDE and LENA Largest Polar/TIDE and IMAGE/LENA outflows ever observed Ion flux ~1.5 x 1010 cm-2s-1 is about 10 x flux for 24-25 Sep 1998

Ionospheric Outflow Processes: 

After Moore, Lundin et al., SSR, 1999 Ionospheric Outflow Processes 1. Solar Wind photothermal 2. Polar Wind photothermal 3. Auroral Wind dissipative coupling of solar wind energy

Ionospheric Global Circulation: 

Ionospheric Global Circulation After Hultqvist, et al. SSR, 1999 Heliosphere: outer magnetosphere and dynamo Geosphere: inner magnetospheric load Magnetosphere: electrodynamic coupler of dynamo to load with feedback

Heliosphere and Geosphere: 

Heliosphere and Geosphere Full 3D computations have taken us from cartoons into simulations. Initial efforts placed all ionospheric dissipation in the F layer, as a boundary condition to the simulations Recent innovations include ionospheric plasma fluids After Winglee, JGR, 1998

Polar Wind and Plasmasphere: 

Polar Wind and Plasmasphere Detailed dynamics of the extended light ion accumulation in the plasmasphere from the IMAGE mission. Basic features understood as effect of enhanced global sunward convection. Features such as spokes, ridges, sub-corotation point toward full simulations as dynamic element of the system Goldstein, et al. JGR, 2002

Cold Plasma Plumes at M’pause: 

Cold Plasma Plumes at M’pause Cold plasmas routinely present in the dayside magnetopause region, convecting according to IMF Densities increase to ~50 cm-3 during sunward flows Likely to load dayside reconnection via local depression of VA Chen and Moore, JGR, 2006

Quantifying Auroral Outflows : 

Quantifying Auroral Outflows IMF and Pd relations are inadquate to specify full spatio-temporal dynamics FAST/Polar Empirical: Ion heating: Friction (300 km) ICW (3000 km) Electron heating: Soft e- (300 km) Hard e- (100 km) “Centrifugal” (pickup 10000+km) Strangeway et al., 2005; Zheng et al., 2005

Dynamic Solar Wind: SBz Excursion: 

Dynamic Solar Wind: SBz Excursion

Dynamic Polar Wind: SBz Excursion: 

Dynamic Polar Wind: SBz Excursion

Dynamic Boundary Conditions: SBz Excursion: 

Dynamic Boundary Conditions: SBz Excursion

Dynamic Auroral Wind: SBz Excursion: 

Dynamic Auroral Wind: SBz Excursion

Substorm O+ ENA: Data - Model: 

Substorm O+ ENA: Data - Model HENA O 50-180 keV 28 October 01 Simulated O ENA Simulated O+ 12:34 UT 12:55 UT 13:30 UT <-- 21 min. --> <-- 35 min. --> <-- 52 min. --> <-- 60 min. -->

Dynamic Solar Wind: Pd Increase: 

Dynamic Solar Wind: Pd Increase

Dynamic Polar Wind: Pd Increase: 

Dynamic Polar Wind: Pd Increase

Dynamic Particle Boundary Conditions: Pd Increase: 

Dynamic Particle Boundary Conditions: Pd Increase

Dynamic Auroral Wind: Pd Increase: 

Dynamic Auroral Wind: Pd Increase

Virtual Spacecraft Dusk Geosync Region: 

Virtual Spacecraft Dusk Geosync Region Integrated over pitch angle

H-G Circulation: 

H-G Circulation A plasma flow chart of the magnetosphere Divided into high latitude (right) and low latitude (left) Solar wind (gold) Polar wind (blue) Auroral wind (green) Qualitative importance (arrow weight)

CONCLUSIONS: 

CONCLUSIONS Largest geospace storms supported by ionospheric ablation Driving auroral wind with local dynamic boundary conditions produces enhanced realism and detail Prolonged NBz shuts down the auroral wind. Substorms are triggered by both SBz, dPd Pre-existing auroral wind O+ outflows are highly compressed by solar wind pressure increase Auroral wind O+ increases with pressure increase, but delayed Future Work Combined SBz and dPd in realistic storm sequences. Simulations with ionospheric plasmas as dynamical elements, e.g. Winglee code, others? Simulations with realistic inner magnetospheric fields, e.g. BatsRUS with CRCM, others?

Backup/Discard Charts: 

Backup/Discard Charts