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Introduction THEMIS instrumentation, orbit and dataset Extended Baseline mission

THEMIS in the inner magnetosphere: Current progress, Future plans and Collaboration with ERG. Introduction THEMIS instrumentation, orbit and dataset Extended Baseline mission THEMIS results in the inner magnetosphere Summary. EFIs. EFIa. SCM. ESA. SST. FGM. T spin =3s.

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Introduction THEMIS instrumentation, orbit and dataset Extended Baseline mission

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  1. THEMIS in the inner magnetosphere:Current progress, Future plans andCollaboration with ERG • Introduction • THEMIS instrumentation, orbit and dataset • Extended Baseline mission • THEMIS results in the inner magnetosphere • Summary

  2. EFIs EFIa SCM ESA SST FGM Tspin=3s Instrument overview Probe instruments: ESA: ElectroStatic Analyzer(coIs: Carlson and McFadden)SST: Solid State Telescopes (coI: Larson)FGM: FluxGate Magnetometer(coIs: Glassmeier, Auster & Baumjohann)SCM: SearchCoil Magnetometer (coI: Roux) EFI: Electric Field Instrument (coI: Bonnell)

  3. THEMIS Extension (FY10,11,12)

  4. Extended THEMIS Baseline (P3,P4,P5) • At the Magnetotail, Study: • Nature of the near-Earth current sheet • Dissipation of bursty fast flows • Result: • Ability to map and model keyinstability region • With first ever: • Simultaneous dR-dZ separations, 0.1-1RE • Clustered orbits study the 8-12RE region Z 2010-04-10 00:00:00 FAST P4 P3 X X P5 Y

  5. P4 P3 P5 Extended THEMIS Baseline (P3,P4,P5) • At Inner Magnetosphere, Study Role of: • ULF/VLF/EMIC waves on ion, electron energization/losses • Large electric fields on storm time ring current • Result: • Comprehensive AC waves and E-fields models • Using novel: • 0.1-2RE separations to resolvetemporal/spatial evolution of gradients • daily conjunctions: PFISR, S-DARN

  6. 2010-04-10 00:00:00 Z P4 P3 X P5 [THEMISCoast PhaseMozer et al.GRL] Extended THEMIS Baseline (P3,P4,P5) • At Subsolar Magnetopause, study: • Asymmetric reconnection: dynamics, evolution and role of cold ions • Internal FTE structure and electron acceleration • Result: • Hall-physics of subsolar magneto-pause reconnection, paves way to MMS • Using novel: • Simultaneous dR-dZ separations at 0.1-0.5RE monitor inflow and outflow • Cluster-like separations at subsolar region

  7. 1 2 3 Usanova et al.,GRL, 2008 EMIC waves • - Driven by SW Pdyn • - Confined to L=5-6.5 • - Structured, with good ground-space correlation

  8. Wang et al.,GRL, 2008 Ring Current Ions Electrons Dst storm index TH-B TH-B TH-D TH-D TH-B TH-B - Ions penetrate deep into the inner magnetosphere, and remain after storm. - Electrons also come close to Earth, but decay fast after storm recovery.

  9. Substorm InjectionWestward Propagation V ~ 350km/s 97A Angelopoulos et al.,First Results from THEMIS, Space Sci. Reviews, 2008 046 Speed: 1MLT/min

  10. Injection Simulatedas localized pulse Liu, Wenlon et al., JGR, 2008

  11. Plasma SheetInjections Runov et al.,GRL, 2008 Ions, TH-C, B, E Electrons, TH-A • Nose structure, temporal • Electron injection local, transient

  12. Generation ofwhistler emissions Li et al.,JGR, 2008 • Low and upper band chorus emissions correlate with 5-10keV electron anisotropy • 10keV electrons at higher L-shells have sufficient anisotropy to generate observed wave power • 1keV electrons can penetrate deep but don’t have the required anisotropy to generate chorus • Higher plasma density results in higher amplitudes

  13. Cully et al.,GRL, 2008 Whistler emissions • Localized, large amplitude chorus emissions • Bursts of sub-second duration • Greater than100mV/m • L~3.5-5.5; dMLT = 1-3 hrs • Mean/average not good description of wave field

  14. KH-wave driven FLRs:Agapitov et al., JGR, 2008 • KH wave seen by THC,B,D,A • Couples to ULF wave on TH-E • Driven ULF wave is localized • Phase change 180o at peak amplitude

  15. Data availability

  16. Summary • THEMIS already presents significant present capability to measure: • Waves, particles and their interactions from the radiation beltsout to the plasma sheet • Continuous operations from solar min to solar max • Can provide plasma sheet sources, measure ULF, EMIC waves for: • RBSP, ERG, Orbitals and other missions if properly planned • Can provide rapid crosses of radiation belt electron phase space density • Multiple satellites can provide information on phase and group velocity • String of pearls configuration can resolve spatio-temporal ambiguities • COLLABORATION ACTIVITIES CAN START NOW: • Mission planning (orbit studies: phasing and conjunction analysis) • Integrated analysis tools (Ground, THEMIS, and simulation data) • Science-targeted campaign planning, (e.g., whistler mode generation and effects)

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