artemis’s planetary goals 1 june 13, 2008 themis extended phase = themis baseline + artemis...

ARTEMIS’s Planetary Goals 1 June 13, 2008

THEMIS Extended Phase=

THEMIS baseline + ARTEMIS

ARTEMIS Lunar Exploration


• 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


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


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


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


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


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)


THEMIS Extension (FY10,11,12)


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


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


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


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


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


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


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


• 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


• 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

artemis’s planetary goals 1 june 13, 2008 themis extended phase = themis baseline + artemis...

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