ARTEMIS Lunar Exploration THEMIS Extended Phase THEMIS baseline

ARTEMIS Lunar Exploration THEMIS Extended Phase = THEMIS baseline + ARTEMIS’s Planetary Goals 1 June 13, 2008

Overview • THEMIS prime (FY 08, FY 09) – Overview, orbits, examples of data and discoveries • THEMIS Extended Phase (FY 10, FY 11, FY 12) – Extended THEMIS Baseline (3 probes) + ARTEMIS (2 probes) – Acceleration Reconnection, Turbulence and Electrodynamics of the Moon’s Interaction with the Sun • The magnetosphere • The solar wind • The lunar wake – ARTEMIS for Planetary • Exospheric Composition, Sputtering Rates • Crustal fields – wake deformation • Lunar interior sounding • Summary ARTEMIS’s Planetary Goals 2 June 13, 2008

TIME HISTORY OF EVENTS AND MACROSCALE INTERACTIONS DURING SUBSTORMS (THEMIS) PRIME MISSION (FY 08 - FY 09) 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 RESOLVING THE PHYSICS OF ONSET AND EVOLUTION OF SUBSTORMS 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 FIVE PROBES LINE UP TO TIME ONSET AND TRACK ENERGY FLOW IN THE TAIL ARTEMIS’s Planetary Goals 3 June 13, 2008

Mission overview: Constellation in excellent health D 2925 -10 @ CCAS EF Ia EFIs SCM ESA BGS SST Release Mission Ops UCB Ground ARTEMIS’s Planetary Goals 4 FGM Tspin=3 s Probe instruments: ESA: Electro. Static Analyzer (co. Is: Carlson and Mc. Fadden) SST: Solid State Telescopes (co. I: Larson) FGM: Flux. Gate Magnetometer (co. Is: Glassmeier, Auster & Baumjohann) SCM: Search. Coil Magnetometer (co. I: Roux) EFI: Electric Field Instrument (co. I: Bonnell) June 13, 2008

Prime mission orbits (FY 07 -FY 09) TH-B TH-C TH-D TH-E TH-A P 1 P 2 P 3 P 4 P 5 First 10 months (Feb 2007 -Dec 2007) First year baseline orbit (FY 08) 2007 -03 -23 Tail 1 2008 -02 -02 2007 -06 -03 YGSE Dayside 1 2008 -08 -08 Launch= 2007 -02 -17 2007 -07 -15 XGSE 2007 -12 -04 Second year baseline orbit (FY 09) 2007 -08 -30 Tail 2 2009 -02 -18 Dayside 2 2009 -09 -16 ARTEMIS’s Planetary Goals 5 June 13, 2008

Discoveries Sphere Dusk MP Sibeck et al. , GRL, in press Wang et al. , GRL, in press Sheath Liu et al. , GRL, in press ARTEMIS’s Planetary Goals 6 June 13, 2008

New results (1 st tail season) Angelopoulos et al. submitted to: Science (embargo in effect) ARTEMIS’s Planetary Goals 7 June 13, 2008

THEMIS Extension (FY 10, 11, 12) ARTEMIS’s Planetary Goals 8 June 13, 2008

ARTEMIS (P 1, P 2): FY 10, 11, 12 FY 10: Translunar injection FY 11 -12: 6 mo Lissajous + 17 mo Lunar ARTEMIS’s Planetary Goals 9 June 13, 2008

ARTEMIS (P 1, P 2) • In the Magnetosphere, study: • Using the first: – Particle acceleration: X-line or O-line? – Reconnection: 3 D character and global effects – Turbulence: Drivers and effects – Two point: d. X, d. Y measurements – …at scales from ion gyroradius to several RE • Result: – Reveal 3 D distant tail, dynamics • In conjunction with: – Solar wind monitors: • ACE, WIND, STEREO – Inner magnetosphere monitors: • Cluster, Geotail, FAST ARTEMIS’s Planetary Goals 10 June 13, 2008

ARTEMIS (P 1, P 2) • In the Solar Wind, study: • Using first of a kind: – Particle acceleration at shocks – Nature and extent of elusive low-shear reconnection – Properties of inertial range of turbulence • Result: – …two point measurements at scales 1 -10 RE, ideal for study of particle evolution in shocks, at foreshock and inertial range of turbulence – 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 ARTEMIS’s Planetary Goals 11 June 13, 2008

ARTEMIS (P 1, P 2) • At the Moon/Wake: • Using first of a kind: – Study 3 D structure and evolution of wake • Result: – Advance our understanding of wakes at planetary moons, plasma void refilling around large objects (Shuttle, ISS, Hubble). – … to better separate lunar surface and interior signatures in the context of environmental influences ARTEMIS’s Planetary Goals 12 – …two point measurements at scales 0. 1 -10 RE, ideal for twopoint correlations within wake and between wake and solar wind June 13, 2008

ARTEMIS and Lunar Exosphere • Lunar Exosphere: – Study composition, distribution of exospheric ions • Under a variety of solar wind conditions ARTEMIS mass spectrometry of pickup ions plotted as “protons” V , y – Comprehensive instrumentation, ample statistics • Result: – Advance our understanding of lunar exosphere and its variability – Goes beyond WIND observations H+ He+ Solar Wind V , x H 2 O+ S+ ARTEMIS-2 Exospheric Pickup Ion ARTEMIS-1 Hartle et al. , 2005 ARTEMIS’s Planetary Goals 13 June 13, 2008

ARTEMIS and Lunar Surface • Lunar Surface: • Using first of kind: – Study composition and distribution of sputtered ions – Understand crustal magnetic fields, surface charging – Remotely sense surface properties of lunar regolith • Result: – …two point measurements of ions and electrons near the Moon, with unprecedented energy coverage and resolution; beyond LP electron reflectometry capability – Advance our understanding of fundamental plasma interactions with planetary surfaces - with applications to Mercury, moons of Jupiter and Saturn, Pluto, KBOs, asteroids, etc. 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 ARTEMIS’s Planetary Goals 14 June 13, 2008

ARTEMIS and Lunar Interior • Unanswered questions about the lunar interior – – – • • Did the Moon form from a collision of Earth and a Mars size object? How much of the moon formed from Earth and how from the impactor? How deep was the lunar magma ocean? Does the Moon have a core? Previous induction studies (Apollo, LP) support the lunar magma ocean hypothesis but are ambiguous due of low signal/noise ratio ARTEMIS’s unique two point measurements allow us to separate external (inducing) and internal (induction response) fields at a wide range of frequencies, with much higher signal/noise ratio – – – Waves of T~0. 1 -1 hr provide information on crust and upper mantle Waves of T~1 -5 hrs provide information on core (size, conductivity) Study response to lobe perturbations: shocks and North-South crossings P 1 1 Hood et al. 1999, GRL P 2 Core? ARTEMIS’s Planetary Goals 15 June 13, 2008

ARTEMIS and Planetary • In support of LRO: – ARTEMIS provide comprehensive monitoring of Lunar Space Environment – Complements LRO/CRATER measurements below 200 ke. V • Supports LADEE and NAS’s Scientific Content of Exploration of the Moon to: – Understand the lunar atmosphere ARTEMIS’s Planetary Goals 16 June 13, 2008

Summary • THEMIS has delivered on its promises – • Major discoveries from coast phase in GRL, JGR, SSR special issues THEMIS+ARTEMIS: Continue to fully embrace community – All Data/Code Open; Help line: THEMIS_Software_Support; Mirror sites proliferating in US, Europe • ARTEMIS: Important for Heliophysics • ARTEMIS: a new mission with very high science value per dollar – – In novel orbits, with comprehensive instrumentation Has tremendous potential to conduct key Heliophysics science: from the moon Addresses important Planetary questions: of the moon Supports major Lunar program missions (LRO, LADEE) ARTEMIS’s Planetary Goals 17 June 13, 2008