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THEMIS/ARTEMIS Mission Outline in the Next Year and during the Extended Mission

THEMIS/ARTEMIS Mission Outline in the Next Year and during the Extended Mission (as proposed in Senior Review, Feb 21) Vassilis Angelopoulos, David Sibeck, Tony Lui, Krishan Khurana, Andrei Runov, Masaki Fujimoto, James Weygand,

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THEMIS/ARTEMIS Mission Outline in the Next Year and during the Extended Mission

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  1. THEMIS/ARTEMIS Mission Outline in the Next Year andduring the Extended Mission (as proposed in Senior Review, Feb 21) Vassilis Angelopoulos, David Sibeck, Tony Lui, Krishan Khurana, Andrei Runov, Masaki Fujimoto, James Weygand, Andreas Keiling, Larry Kepko, Rumi Nakamura, Alain Roux, John Samson, Victor Sergeev, Zoltan Voros, Tai Phan, Marit Oieroset, David Schriver, Chris Russell,Xinlin Li, Ian Mann, Chris Chaston, Jonathan Eastwood, Jasper Halekas,Pavel Travnicek, Dietmar Krauss-Varban, Forrest Mozer, Bill Farrell, Sabine Frey,Hiroshi Hasegawa, Neil Murphy, Jimmy Raeder, David King and Jim Slavin Special Thanks to our Red Team Reviewers: Nicky Fox, Pontus Brandt, Chris StCyr, Doug Rowland

  2. Mission Planning Status • THEMIS approved as proposed in FY10-12 • With a ~1/3 science budget reduction • Three probes in inner orbits • Performs Cluster-type science in region not visited by Cluster • Detailed planning commences today (now that Tail2 is in check) • ARTEMIS program approved • Funding for operations only, minimal for science team • Heliophysics ARTEMIS GI program (1M/yr x 2 yrs), team can compete for • Requested help from the Planetary Division, first installment received • Expect to submit proposal to Planetary by mid-November for more funds • Costs to defray Ops costs, releasing funds for Heliophysics science • Will enable coI funds for 8 new scientists • A Participating Scientist Program to be bundled with GI (1M/yr x 3yrs ?) • Reviews • Planetary proposal: Mid-November • ARTEMIS Operations Review: December 2008 • Confirmation review: February 2009

  3. Mission at a Glance (SR 2008-Tbl. 1A)

  4. Next (Dawn) Sector Conjunctions • Radiation Belt science triggers were limited before, now can improve • Density trigger works great at M-pause but not in Rad. Belts • Considering waves trigger: FB from SCM, 80Hz – 1kHz band • Radiation Belt Fast Survey increases • Increase duration to 2hrs on either side of Rad. Belts (outside L=4) • Mode changes: • Worth going to higher frequency (16kS/s) and closer (maybe in dusk sector?) • Planning starts week of Sept. 30th • Maneuvers on week of Oct 6th • Rad. Belt new modes proposed to be implemented on week of Oct. 13th

  5. Feb-26 Jan-29 Next (Tail) Season Conjunctions • Learning our lessons from past tail season: • P1, P2 saw tailward flows/beams only when <1RE • P1, P2 saw no dispersed energetic particle beams when >1RE • Only a handful of events (Feb. 16 to Mar. 1) amenable to timing • Yield loss within +/- 1RE due to plasma sheet flapping: <40% • Need to be near neutral sheet (dNS <1RE) to improve substorm statistics. 1st tail season (Jan-Mar 2008) Feb-26 Mar-01 Feb-22 Feb-18 Feb-14 Feb-10 Feb-6 Jan-29 Feb-2 Midnight Pre-midnight

  6. T3 (2010-04-05) D3 (2010-11-01) Y P3 P4 Z P5 P 5 T3, GSE coord’s View from dawn along NS dZ(P3-P5) ~ 600-3000km dR(P3-P4)~1RE > dZ [every 8 days] P4 P3 X Y D3, GSE coord’s View from dawn on Ecliptic dZ(P3-P5) ~ 1000-3000km dR(P3-P4)~1000km < dZ [every day] Apogee~12Re P3,4,5, orbits for T3/D3/R3Separations >0.5RE in dR-dZ Y R3 (Year-round) X Z P5 P3 P4 R3, GSE coord’s View from topdZ(P3-P5), as in T3.Variable along-trackseparations

  7. 1000km P3,4,5 orbits for T4, D4, R4, T5Separations < 0.5RE in dR-dZ T4 (2011-05-10)T5 (2012-06-21) D4 (2011-12-01) Z Z 1000km Y Y X T4 (and T5), GSE coord’s View from dawn along NS dZ(P3-P5) ~ 100-500km dR(P3-P4)~1000km > dZ [every day] Apogee ~ 12RE X D4, GSE coord’s dZ(P3-P5) ~ 1000-3000kmdR(P3-P4)~1000km < dZ[every day] Apogee~12Re R4 (at Dawn/dusk) P5 P4 P3 R4, GSE coord’s View from topString-of-Pearls.Variable along-trackseparations: 100km-2RE

  8. P3,4,5 prime maneuvers and deltaV

  9. 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

  10. 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

  11. 2010-04-10 00:00:00 Z P4 P3 X P5 [THEMISCoast PhaseMozer et al.GRL 2008] 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

  12. THEMIS Extension (FY10,11,12)

  13. P1 raise starts Aug 1, 2009P2 raise starts July 1, 2009 Translunar injectionin September 2009 Take what you canfor 2nd dayside science during orbit raise(loss minimal) Phase I (Oct ’09 – Oct ’10) - placement P2 P1

  14. ARTEMIS Selective Orbits Phase II (Oct ’10 – Jan ’11) – opposite

  15. ARTEMIS Selective Orbits Phase II (Oct ’10 – Jan ’11) – opposite

  16. ARTEMIS Selective Orbits Phase III (Jan ’11 – Apr ’11) – same side

  17. Phase III (Jan ’11 – Apr ’11) – same side

  18. Phase III (Jan ’11 – Apr ’11) – same side

  19. ARTEMIS Wake Crossings: Phase II,III

  20. ARTEMIS Distant Wake Crossings:A Perspective dB

  21. Phase IV (Apr ’11 – Sep ’12) ARTEMIS After Insertion

  22. ARTEMIS Wake Crossings

  23. ARTEMIS Fuel Margin

  24. ARTEMIS Tail Science (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

  25. ARTEMIS Solar Wind Science (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

  26. ARTEMIS Wake Science (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

  27. Dust Levitation in Electric Fields Apollo observers saw dust elevated above the lunar surface to possibly high altitudes. LADEE will probably have a dust detector, but has no capability of measuring the solar wind electric and magnetic fields. ARTEMIS measures the solar wind velocity, the interplanetary magnetic field and hence the solar wind electric field. It also can measure surface potentials with electron reflectometry. ARTEMIS plus LADEE will enable us to determine the response of charged lunar dust to the lunar and solar wind electric fields. ARTEMIS Planetary Science (P1,P2) LADEE ARTEMIS-1 ARTEMIS-2 27

  28. ARTEMIS and Lunar Exosphere ARTEMIS mass spectrometryof pickup ions assumed “protons” • Apollo’s ALSEP package contained a suprathermal ion detector (SIDE) that detected ions accelerated by electric field toward lunar surface.WIND observations confirmed presence of heavy ions around moon. • Temporal history of ion fluxes on SIDE suggested that the moon might be episodically outgassing. Alpha particle observations of localized concentrations of radon also support this viewpoint. • This observation needs confirmation. If true, there may be a source of lunar volatiles at low latitudes, not just at the poles. • ARTEMIS has an ion detector and measures the solar wind electric field so it can test the SIDE hypothesis of an outgassing moon. V,y H+ V,x He+ H2O+ S+ Solar Wind ARTEMIS-2 Exospheric Pickup Ion ARTEMIS-1 Hartle et al., 2005

  29. ARTEMIS and Lunar Surface • Lunar Surface: • Study composition and distribution of sputtered ions • Understand crustal magnetic fields, surface charging • Remotely sense surface properties of lunar regolith • Result: • Advance our understanding of fundamental plasma interactions with planetary surfaces. • Using first of kind: • …two point measurementsof ions and electrons near the Moon, with unprecedented energy coverage and resolution; beyond LP electron reflectometry capability Secondary electrons measured by Lunar Prospector [Halekas et al. 2008] Trace sputtered ions back to lunar surface ARTEMIS Secondary and photo-electrons accelerated from charged lunar surface reveal regolith surface properties

  30. Interior Structure of the Moon Apollo orbital measurements provided evidence of an iron core of about 400 km radius. Lunar Prospector made similar (single instrument) measurements and confirmed the Apollo subsatellite result. Two-point measurements are needed to go beyond the current two-layer model of the interior electrical conductivity. ARTEMIS will provide measurements of both the “exciting” field and the resulting induced magnetic field at about 100 km over a range of frequencies and sound the electrical conductivity profile above the core. P1 P2 Core? 30

  31. ARTEMIS and Planetary, Summary • In support of LRO: • ARTEMIS can provide comprehensive monitoring of Lunar Space Environment • Complements LRO/CRATER providing measurements below 6MeV • Note: ARTEMIS has been already supporting LRO via White Sands G/N testing • Supports NAS’s Scientific Content of Exploration of the Moon to: • Understand the lunar atmosphere • In support of all missions • ARTEMIS provides comprehensive monitoring of plasma conditions and lunar surface electric fields • Allows study of the response of the lunar exosphere and dust to external drivers • ARTEMIS provides solar wind monitoring

  32. THEMIS/ARTEMIS Outlook Senior review to finalize FY11-12 budget expected in 1.5yrs (due Feb 10), based on team publications. Opportunities for extended mission beyond 2012 are good but the level depends solely on the team’s productivityand the quality of research from the prime missionand the first extension !

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