living with a star radiation belt storm probes and associated geospace missions d. g. sibeck project...
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Living With a Star Radiation Belt Storm Probes and Associated
Geospace Missions
D. G. Sibeck
Project ScientistNASA Goddard Space Flight Center
Geospace: Part of the Integrated LWS Plan
Distributed network of spacecraft providing continuous observations of Sun-Earth system Solar and Heliospheric Network observing the Sun & tracking disturbances from the Sun to Earth
Geospace Network uses a comprehensive set of spacecraft to diagnose the Geospace response
Stereo Lag
Stereo Lead
Solar Probe
• •Radiation Belt Storm Probes•Ionosphere-Thermosphere Storm Probes•UV Imager: O/N2 and Electron Density•SDO observations of EUV input
Original Geospace Mission Concept
The Radiation Belt Storm Probes Mission is in Phase A Formulation
Radiation Belt Storm Probes – twin spacecraft in highly elliptical orbits to understand the basic principals behind relativistic particle acceleration, transport, and loss.
Launch 2012Perigee: ~630 km altitudeApogee ~5.8 Re geocentric altitudeInclination ~10°Sun pointing, spin stabilizedDuration 2 years (expendables 4 years)
•Physics of the radiation belts are the physics of•Charge particle acceleration, transport, and loss.
Radiation Belts:Our Window on Fundamental Physics
• Source, loss, and transport processes
• Shock-associated creation and decay of radiation belts;
• Quantifying adiabatic and nonadiabatic processes;
• ”Seed" or source populations;
• Ring current and its effects on energetic particles;
• Data assimilation and specification models --> for practical applications
LWS Geospace RBSP Study Objectives
Mission Approach
•Simultaneous two-point measurements by
• identical spacecraft in common orbits.
•with a slow separation in phase,
•lapping one another 4-5 times/year,
•Covering the full range of local times in 2 years.
•Apogee of ~ 5.8 Re to sample outer belt and ring current.
•Perigee of ~ 630 km to sample inner belt.
•Simultaneous two-point measurements by
• identical spacecraft in common orbits.
•with a slow separation in phase,
•lapping one another 4-5 times/year,
•Covering the full range of local times in 2 years.
•Apogee of ~ 5.8 Re to sample outer belt and ring current.
•Perigee of ~ 630 km to sample inner belt.
plasmasphere
outer radiationbelt
1
23
Precession
Radial Profiles -->Distinguish Mechanisms
•When closely spaced-->
• determine radial phase space density gradients and discriminate between proposed source/loss regions and processes.
Convection
RadialDiffusion
LocalAcceleration
Spatial Extent
•When widely separated -->
•measure spatial extent of ring current asymmetries and wave fields.
Identify Source Populations
•Measure ‘seed’ or source populations: Plasma sheet Substorm injected plasma Pre-existing relativistic particles Solar Energetic Particles.
•and accelerated populations simultaneously.
4. Selected Investigations
• NASA/HQ selected the following experiments:– ECT (Spence, Boston U.) Energetic Particle Composition
and Thermal Plasma Suite– EMFISIS (Kletzing, U. Iowa) Electric and Magnetic Field
Instrument Suite and Integrated Science– EFW (Wygant, U. Minnesota) Electric Field and Waves
Instrument for the NASA RBSP Mission– RBSPICE (Lanzerotti, N.J. Inst. Technology) Radiation Belt
Storm Probes Ion Composition Experiment
• NASA entered into a partnership agreement with the NRO, who will supply:– RPS (Groves) Relativistic Proton Spectrometer
Three Missions of Opportunity in Competitive Phase A Study
GOLD MOREBARREL
Robyn Millan Dartmouth College
Balloon Array for RBSP Relativistic Electron
Losses
Daniel Baker
U. Colorado Boulder
Mission of Opportunity RadBelt Experiment
Richard EastesU. Central Florida
Global-scale Observations of Limb
and Disk
–Final reports due September 12, 2007
–Result could augment RBSP and/or IT science.
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