artemis’s planetary goals 1 june 13, 2008 themis extended phase = themis baseline + artemis...
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ARTEMIS’s Planetary Goals 1 June 13, 2008
THEMIS Extended Phase=
THEMIS baseline + ARTEMIS
ARTEMIS Lunar Exploration
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ARTEMIS’s Planetary Goals 2 June 13, 2008
• THEMIS prime (FY08, FY09)– Overview, orbits, examples of data and discoveries
• THEMIS Extended Phase (FY10, FY11, FY12)– 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
Overview
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ARTEMIS’s Planetary Goals 3 June 13, 2008
TIME HISTORY OF EVENTS AND MACROSCALE
INTERACTIONS DURING SUBSTORMS (THEMIS)
RESOLVING THE PHYSICS OF ONSET AND EVOLUTION OF SUBSTORMS
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 FIVE PROBES LINE UP TO TIME ONSET AND TRACK ENERGY FLOW IN THE TAIL
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ARTEMIS’s Planetary Goals 4 June 13, 2008
Mission overview: Constellation in excellent health
BGS
Mission OpsUCB
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)
Ground
SST
ESA
EFIa
EFIs
FGM
SCM
Tspin=3s
Release
D29
25-1
0 @
CC
AS
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ARTEMIS’s Planetary Goals 5 June 13, 2008
Launch=2007-02-17
2007-03-23
2007-06-03
2007-07-15
2007-08-302007-12-04
XGSE
YGSE
TH-B
TH-C
TH-D
TH-E
TH-A
P1
P2
P3
P4
P5
First 10 months(Feb 2007-Dec 2007) First year baseline orbit (FY08)
Second year baseline orbit (FY09)
Prime mission orbits (FY07-FY09)
Dayside 12008-08-08
Tail 12008-02-02
Dayside 22009-09-16
Tail 22009-02-18
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ARTEMIS’s Planetary Goals 6 June 13, 2008
Discoveries
13.0
12.5
12.0
11.5
11.0
10.5
10.0
Y (
R E)
8.0 7.5 7.0 6.5 6.0 5.5 5.0
X (RE)
Magnetosphere
Magnetosheath
30 nT
20 nT
10 nT13.0
12.5
12.0
11.5
11.0
10.5
10.0
Y (
R E)
8.0 7.5 7.0 6.5 6.0 5.5 5.0
X (RE)
A
ED
C
B
Bxy
Dusk MP
Sphere
Sheath
Sibeck et al.,GRL, in press
Wang et al.,GRL, in press
Liu et al.,GRL, in press
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ARTEMIS’s Planetary Goals 7 June 13, 2008
New results (1st tail season)
P 2 P 1P 3P 4
P 5 T =0Rx
x
X [R ]GSM E
Z [R
]G
SM
E
T =182sCD
T =96sON
T =138sE X M agne to tail lobe
P lasm a shee tN eutral shee t
Angelopoulos et al. submitted to: Science (embargo in effect)
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ARTEMIS’s Planetary Goals 8 June 13, 2008
THEMIS Extension (FY10,11,12)
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ARTEMIS’s Planetary Goals 9 June 13, 2008
Lunar WakeFormation/Evolution
Diffusive Particle
Acceleration
Shock tangent
Foreshock waves
Turbulent wake?
Last closed field lineGeotail
THEMISMoon
P1P2
P1 P2Solar Wind
X
Magnetotail
ARTEMIS (P1,P2): FY10,11,12
FY10: Translunar injectionFY11-12: 6mo Lissajous + 17 mo Lunar
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ARTEMIS’s Planetary Goals 10 June 13, 2008
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
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ARTEMIS’s Planetary Goals 11 June 13, 2008
ARTEMIS (P1,P2)
• Using first of a kind:– …two point measurements
at scales 1-10 RE, ideal for study of particle evolution in shocks, at foreshock and inertial range of turbulence
• 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
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ARTEMIS’s Planetary Goals 12 June 13, 2008
ARTEMIS (P1,P2)
• At the Moon/Wake:– Study 3D 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 interiorsignatures in the context of environmental influences
• Using first of a kind:– …two point measurements
at scales 0.1-10 RE, ideal for two-point correlations within wake and between wake and solar wind
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ARTEMIS’s Planetary Goals 13 June 13, 2008
ExosphericPickupIon
ARTEMIS-1
ARTEMIS-2
H+
He+H2O+ S+
ARTEMIS mass spectrometryof pickup ions plotted as “protons”
V,x
V,y
Solar Wind
• Lunar Exosphere:– Study composition, distribution of exospheric ions
• Under a variety of solar wind conditions
– Comprehensive instrumentation, ample statistics
• Result:– Advance our understanding of lunar
exosphere and its variability– Goes beyond WIND observations
ARTEMIS and Lunar Exosphere
Hartle et al., 2005
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ARTEMIS’s Planetary Goals 14 June 13, 2008
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 - with applications to Mercury, moons of Jupiter and Saturn, Pluto, KBOs, asteroids, etc.
• Using first of kind:– …two point measurements
of ions and electrons near the Moon, with unprecedented energy coverage and resolution; beyond LP electron reflectometry capability
Trace sputtered ionsback to lunar surface
Secondary and photo-electronsaccelerated from charged lunar surfacereveal regolith surface properties
Secondary electronsmeasured by LunarProspector [Halekas et al. 2008]
ARTEMIS
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ARTEMIS’s Planetary Goals 15 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~0.1-1hr 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
Hood et al. 1999, GRL
1
Core?
P1 P2
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ARTEMIS’s Planetary Goals 16 June 13, 2008
• In support of LRO:– ARTEMIS provide comprehensive monitoring of Lunar Space Environment– Complements LRO/CRATER measurements below 200keV
• Supports LADEE and NAS’s Scientific Content of Exploration of the Moon to:– Understand the lunar atmosphere
ARTEMIS and Planetary
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ARTEMIS’s Planetary Goals 17 June 13, 2008
• 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)
Summary