THEMIS and ARTEMIS Status

In summary Senior Review 2010 Results Good: THEMIS extended through 2014 (with small decline in 2013-2014) ARTEMIS extended through 2014 as well (details pending) Expect new /revised contract with GSFC to account for uptick due to ARTEMIS Plan to have visiting scholars (6mo. to 1yr) at UCLA, UCB Only negative was SST calibration. Plans taken to: Offload work from Davin who is busy on Maven, SP+ Perform calibrations, modeling at UCLA Mirror some efforts at UCB on Maven Plan to ramp up inner magnetosphere activities Plan to continue with mode adjustments for ARTEMIS

THEMIS Extension (FY10,11,12)

FY 10/11/12 FY 13/14 Extended Mission: THEMIS probe separations Kinetic: 100km – 5000km Global: 2RE – 8RE FY 10/11/12 FY 13/14 2010-04-10 00:00:00 2010-04-10 00:00:00 Tail or Dayside Z Z P5 P4 P4 P3 X or -X X or -X Inner magnetosphere P5 P3 FY13: 4-8-12 hrs P3 FY14: 8-8-8 hrs

Tail from kinetic scales: FY11/12 Interaction of reconnection jet (or dipolarization front) with the inner magnetosphere and its role in triggering substorms THEMIS Burst data Bz P1 (nT) Bz P2 Z (nT) FY 11/12 objective: Physics of interaction between flow bursts and inner magnetosphere (injections?) Bz P3 Jy ~ 100 nA/m2 X (nT) z P3 P4 intense waves E (Hz) P3 z x P5 P3 30 keV electrons (f) 95 keV Runov et al. [2010]

Subsolar magnetopause from kinetic scales: FY11/12 Microphysics of asymmetric reconnection, pathfinder for MMS North-south asymmetry in asymmetric reconnection Evolution of reconnection layer with increasing distance from X-line 2010-04-10 00:00:00 P3 P4 P5 X Z Electron jet only north of X-line Z separation = 1000-3000 km = 10-30 ion skin depths Pritchett and Mozer [2009]

Phase Space Density (PSD) Inner magnetosphere kinetic processes: FY11/12 Role of waves in particle acceleration/loss An RBSP pathfinder as solar max ramps up Convection Radial Diffusion Local Acceleration * * * THEMIS spacecraft observe: Plasma distributions generating waves Waves responsible for acceleration/scattering/loss Electric fields that transport particles Magnetic fields that guide particle motion And thus: Separate spatial from temporal effects Determine spatial extent of sources/sinks Quantify radial PSD gradients Distinguish between competing models Phase Space Density (PSD) * * * * * * Radius (L-shell)

Inner magnetosphere: FY13/14 The global view at Solar Max Exploring the relationship between particle sources/sinks and the inner magnetosphere An RBSP partner, continuously monitor sources/sinks at 12RE Broadly-spaced THEMIS spacecraft observe: Source region plasmas and fields Other radiation belt drivers: transmitted shocks, pressure pulses, boundary layer waves and substorm injections ..thus constraining radiation belt models FY 11/12 (Gaps) FY13/14 (Gaps Filled)

ARTEMIS (P1 and P2) Angelopoulos, 2010 Sibeck et al., 2010 Lissajous Phase (Oct ’10 – Apr Jul’11) Note: First 3 months: opposite sides, Next 3 months: same side Translunar injection phase (Oct ’09 – Oct ’10) Note 1: Orbit Raise Maneuvers (ORMs) completed flawlessly, targeting complete! Lunar Orbit Phase (AprJul ’11 – Sep ’12) Note: P1 retrograde, and P2 prograde, such that orbital separations and separation vectors cover full parameter space Angelopoulos, 2010 Sibeck et al., 2010 Halekas et al., 2010 Bester et al., 2011 Swetser et al., 2011

Magnetotail In the Magnetosphere, study: Result: In conjunction with: 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: THEMIS, Cluster and Geotail Using the first: Two point: dX, dY measurements …at scales from ion gyroradius to several RE

Solar Wind/Wake First Flyby When Moon is in the Solar Wind: Seed population for solar energetic particles Nature of elusive low-shear reconnection Properties of inertial range of turbulence Near the Moon (Wake): Structure and evolution of lunar wake Particle acceleration and dynamics at wake Moon as an analogue for other airless bodies Using first of kind: …two point measurements at scales 0.1-10 RE, ideal for two-point correlations within wake and between wake and solar wind Bonus!! Solar wind monitor for lunar and other heliophysics science ARTEMIS First Flyby Moon/ ARTEMIS

Wake Update: First Flyby! Models converging, still lots to understand Models help identify alphas and protons Models identify exiting electron beam as accelerated penetrating core/halo electrons from entry side Models predict similar beam on entry side which is not clearly observed 0-15° 165-180° Spectra Corrected for S/C Potential

ART-THM conjunction P5 P1 P2 P3 P2 P3,4,5 P4 P1

In short Many more discoveries from THEMIS and ARTEMIS together expected. Analysis tools in conjunction wth ERG and SD are being developed. Knowledge gained in the next 2 years will set the stage for RBSP and MMS. THEMIS plans to position its instrument modes and orbits to collaborate with both missions.