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THEMIS Extended Phase = THEMIS baseline + ARTEMIS

THEMIS Senior Review. THEMIS Extended Phase = THEMIS baseline + ARTEMIS. Overview. THEMIS prime (FY08, FY09) Overview, orbits Accomplishments to-date New results from first tail season Beyond the substorm trigger THEMIS Extended Phase (FY10, FY11, FY12)

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THEMIS Extended Phase = THEMIS baseline + ARTEMIS

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  1. THEMIS Senior Review THEMIS Extended Phase = THEMIS baseline + ARTEMIS

  2. Overview • THEMIS prime (FY08, FY09) • Overview, orbits • Accomplishments to-date • New results from first tail season • Beyond the substorm trigger • THEMIS Extended Phase (FY10, FY11, FY12) • Extended THEMIS Baseline (3 probes) • Magnetotail science • Inner magnetosphere • Dayside science • ARTEMIS (2 probes) Acceleration Reconnection, Turbulence in… • The magnetosphere • The solar wind • Electrodynamics of the Moon’s Interactions with the Sun. • Summary

  3. TIME HISTORY OF EVENTS AND MACROSCALE INTERACTIONS DURING SUBSTORMS (THEMIS) • PRIME MISSION (FY08 - FY09) SCIENCE GOALS: • Primary: • “How do substorms operate?” • One of the oldest and most important questions in Geophysics • A turning point in our understanding of the dynamic magnetosphere • First bonus science: • “What accelerates storm-time ‘killer’ electrons?” • A significant contribution to space weather science • Second bonus science: • “What controls efficiency of solar wind – magnetosphere coupling?” • Provides global context of Solar Wind – Magnetosphere interaction RESOLVING THE PHYSICS OF ONSET AND EVOLUTION OF SUBSTORMS FIVE PROBES LINE UP TO TIME ONSET AND TRACK ENERGY FLOW IN THE TAIL

  4. EFIs EFIa SCM ESA BGS SST Mission Ops UCB FGM Tspin=3s Ground Mission overview: Constellation in excellent health D2925-10 @ CCAS Release 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)

  5. P1 P2 P3 P4 P5 TH-B TH-C TH-D TH-E TH-A Prime mission orbits (FY07-FY09) First 10 months(Feb 2007-Dec 2007) First year baseline orbit (FY08) 2007-03-23 Tail 12008-02-02 2007-06-03 YGSE Dayside 12008-08-08 Launch=2007-02-17 2007-07-15 XGSE Second year baseline orbit (FY09) 2007-08-30 2007-12-04 Tail 22009-02-18 Dayside 22009-09-16

  6. Status • Probes, instruments function nominally; team in place • Data collected per plan, widely disseminated • Mirror sites in Japan, France, Austria, Taiwan, Canada, China • Data in CDF, IDL analysis routines available, VMO/SPASE-compliant • Software Support, Tutorials on-line and Demos at meetings • Pressure for publications and discovery by NASA: huge! • Science discoveries piling up • 40 science papers in last AGU conference • Numerous papers in Intl. Conf. on Substorms #9 (Graz, Austria) • >12 Space Science Review papers in review or in press • >16 GRL papers accepted (25% non-coI team, 40% students or post-docs) • >20 JGR papers in process • Minimum mission accomplished (First tail season) • > 50 substorms collected • Optimal data between Feb 15th - Mar 10th • Data already collected solve substorm trigger problem • Second tail season: ionospheric coupling, statistics and further insight • Constellation in good health ready for extended mission planning

  7. First dissection of a detached FTE Sphere Dusk MP Sheath Discoveries Birth of storm-time ring current Sibeck et al.,GRL, in press Wang et al.,GRL, in press Liu et al.,GRL, in press First detection of remote signatures of FTE's: Dayside Traveling Compression Regions

  8. Substorm trigger identified New results (1st tail season) Angelopoulos et al. submitted to: Science (embargo in effect)

  9. Beyond Substorm Timing, 2nd tail (FY09) + • Complete prime mission 2nd year tail: • Macroscale interactions: flow diversion or tailward retreat of X-line ? • Means of ionospheric coupling • Coupling to local instabilities: ballooning, whistler modes • Statistics of triggers under a variety of solar wind conditions • Do externally (solar wind) triggered onsets differ from spontaneous ones? • Beyond prime: resolve open questions on substorms: • What causes gradual auroral brightening ahead of onset? • What process enables the current sheet to reconnect? • Does tail history dictate onset mechanism, location? • Extended mission is ideally positioned to go beyond timing studies • Pace of discoveries, and progress expected to accelerate

  10. THEMIS Extension (FY10,11,12)

  11. ARTEMIS (P1,P2): FY10,11,12 FY10: Translunar injection FY11-12: 6mo Lissajous + 17 mo Lunar

  12. 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 Courtesy: Pulkkinen and Wiltberger

  13. 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

  14. 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

  15. ARTEMIS (P1,P2) • In the Magnetosphere, study: • Particle acceleration: X-line or O-line? • Reconnection: 3D character and global effects • Turbulence: Drivers and effects • Result: • Reveal 3D distant tail, dynamics • In conjunction with: • Solar wind monitors: • ACE, WIND, STEREO • Inner magnetosphere monitors: • Cluster, Geotail, FAST • Using the first: • Two point: dX, dY measurements • …at scales from ion gyroradius to several RE

  16. ARTEMIS (P1,P2) • In the Solar Wind, study: • Particle acceleration at shocks • Nature and extent of elusive low-shear reconnection • Properties of inertial range of turbulence • Result: • Advance our understanding of particle acceleration and turbulence in Heliosphere • In conjunction with: • Other solar wind monitors: • ACE, WIND, STEREO • ARTEMIS is: • High-fidelity solar wind monitor • In beacon mode if requested • Using first of a kind: • …two point measurementsat scales 1-10 RE, ideal for study of particle evolution in shocks, at foreshock and inertial range of turbulence

  17. ARTEMIS (P1,P2) • At the Moon/Wake: • Study 3D structure and evolution of wake • Understand particle acceleration processes at wake • Understand wake refilling for various SW conditions • Result: • Advance our understanding of wakes at planetary moons, plasma void refilling around large objects (Shuttle, ISS, Hubble) • Using first of a kind: • …two point measurementsat scales 0.1-10 RE, ideal for two-point correlations within wake and between wake and solar wind

  18. Summary • THEMIS has delivered on its promises • Major discoveries from coast phase in GRL, JGR, SSR special issues • Minimum mission accomplished, substorm trigger identified, to be solidified by 2nd year statistics • Major discoveries from 1st tail season to appear in Science, JGR, Annales Geophysicae • THEMIS to dominate in Intl. Substorm Conference #9 • THEMIS+ARTEMIS: Continue to fully embrace community • All Data Open in CDF, IDL Analysis Code on-line, VMO/SPASE • Help line: THEMIS_Software_Support; Quality Controlled Code updates • Mirror sites proliferating in US, Europe and Asia • Software tutorials at main meetings • Papers by non-team members already in press • THEMIS+ARTEMIS: Can Form Cornerstone of Heliophysics Observatory • In novel orbits, with comprehensive instrumentation, address pressing Heliophysics questions • THEMIS baseline = Clustered at equatorial magnetosphere: uniquely suited to address current dynamics, dissipation • ARTEMIS = Two probes, address fundamental physics in Tail, Solar wind and at the Lunar distances • A bridge in Heliophysics discipline, between ISTP+Cluster era and RBSP, MMS era • Complement existing missions and provide context for new ones (e.g., RBSP)

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