EGU General Assembly 2006, 2-7 April, 2006, Wien EGU General Assembly 2006, 2-7 April, 2006, Wien ST6 Multi-point measurements of solar-terrestrial plasma: results and future perspectives ST6 Multi-point measurements of solar-terrestrial plasma: results and future perspectives Scientific objectives and Scientific objectives and opportunities during THEMIS opportunities during THEMIS mission mission R. Nakamura, V. Angelopoulos, W. Baumjohann, E. Donovan 1. Overview of THEMIS mission 2. What can we do more if we add Cluster/Ground-based observations (in European sector) to THEMIS ?
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EGU General Assembly 2006, 2-7 April, 2006, Wien ST6 Multi-point measurements of solar-terrestrial plasma: results and future perspectives Scientific objectives.
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EGU General Assembly 2006, 2-7 April, 2006, Wien EGU General Assembly 2006, 2-7 April, 2006, Wien ST6 Multi-point measurements of solar-terrestrial plasma: results and future ST6 Multi-point measurements of solar-terrestrial plasma: results and future
perspectivesperspectives
Scientific objectives and Scientific objectives and opportunities during THEMIS opportunities during THEMIS
missionmission
R. Nakamura, V. Angelopoulos, W. Baumjohann, E. Donovan
1. Overview of THEMIS mission
2. What can we do more if we add Cluster/Ground-based observations (in European sector) to THEMIS ?
Acknowledgements: S. Apatenkov, S. Frey, V. Sergeev, O. Amm, A. Grocott, NASA GSFC/SPDF
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THEMISTIME HISTORY OF EVENTS AND MACROSCALE INTERACTIONS DURING SUBSTORMS
Principal InvestigatorVassilis Angelopoulos,UCBProject ManagerPeter Harvey, UCB
Primary SCIENCE GOAL:“How do substorms operate?”
Launch planned in October 2006
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THEMIS team and instrumentsTHEMIS team and instrumentsScience Team
SST
ESA
EFIaEFIs
FGM
SCM
Tspin=3s
Probe instruments:ESA: Thermal plasmaSST: Super-thermal plasmaFGM: Low frequency magnetic fieldSCM: High frequency magnetic fieldEFI: Electric field
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Orbits designed for ideal conjunction with GBO
Substorm onset locations, Substorm onset locations, THEMIS footprints, and GBO keogramsTHEMIS footprints, and GBO keograms
FUV KEOGRAMKIANA195+/-5 deg. longitude
FUV KEOGRAMGILLAM260+/-5 deg. longitude
FUV KEOGRAMGOOSE295+/- 5 deg. longitude
P1 footprintsP2 footprints
P3,4 footprints
P5 footprints
[Frey et al., 2005]
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How do substorm operate ?How do substorm operate ?
P1P2P3P4P5
GBO
Flows
?Rarefaction wave
?
Timing between current disruption, reconnection and ground onset withing 30s time resolution
Macroscale Interactions (causal relationship)
Ionospheric coupling
THEMIS covers all key regions of a substorm
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THEMIS and ClusterTHEMIS and Cluster
Apogee 2007:
Winter: Tail-Cusp
Spring: Dusk-Dawn Flanks
Summer: Tail-LLBL
Fall: Dawn-Dusk Flanks
Courtesy MA Hapgood, Rutherford Laboratory,UK
What can we do more if we add Cluster/Ground-based observations (in European sector) to THEMIS ?
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Ionospheric disturbances associated with fast flows can be identified as:
Enhanced local convection pattern
Experience from Cluster-GB studyExperience from Cluster-GB study
Ionospheric/field-aligned current modification
[Grocott et al., 2004] [Nakamura et al., 2005]
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Orbit is designed for North Orbit is designed for North America.. BUTAmerica.. BUT
there are orbits favorable for European sector.
dense ground-based network can be used
Cluster1
Cluster4
THEMIS 1
THEMIS 2THEMIS 5
THEMIS 3
THEMIS 4
Multi-point satellite-ground based studies using THEMIS&Clusterand dense ground-based network can be performed in 2006/2007 winter season
Acknowedgement: NASA/SSCWeb
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Experience from Cluster-DSP studyExperience from Cluster-DSP studyStory may be more complex: Energy dissipation via Alfvén waves? [e.g., Nakamura et al., 2005]
THEMIS’s 3D electric field measurementsmay be able to answer this question as well
Evolution of BBF is yet to be understood
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Cluster perigee observation during Cluster perigee observation during BBFBBF
2004/02/23 3 :20-3:30U T XZgsm p lane, fie ld lines T89, Kp=0SC locations are show n: LA N L1990 ---- 0 .5M LT;C luster 1 ,2 ,3,4 --- 0 .8M LT; G O ES12 --- 22M LT; G eota il --- m idn ight
Cluster (in pearl-on-string configuration, 1>3>2>4)
THEMIS (Launch: October 2006) will provide ideal plat forms to study large-scale substorm physics, plasma transport/acceleration processes and solar wind-magnetosphere interaction.
Coordinated observations with Cluster/DSP and dense ground-based observations in European sector will allow even more science returns.