An Auroral Imaging Mission for ILWS Eric Donovan - University of Calgary December 9, 2004 Acknowledgements: John Bonnell & Emma Spanswick Representing: Trondsen, Murphree & Cogger (Calgary) & Jamar (CSL)

L. Cogger University of Calgary E. Donovan University of Calgary J.C. Gérard Université de Liège M. Henderson Los Alamos National Laboratory C. Jamar Centre Spatiale de Liège P. Jayachandran University of Western Ontario K. Kabin University of Alberta K. McWilliams University of Saskatchewan J.S. Murphree University of Calgary T. Pulkkinen Finnish Meteorological Institute R. Rankin University of Alberta J. Rae University of Alberta P. Rochus Centre Spatiale de Liège G. Sofko University of Saskatchewan T. Trondsen University of Calgary Science Team 2004/12/09

Ravens The “Quaff B” Scenario Quaff A at L1 Quaff B “Ravens +” The Quaff mission could incorporate the Ravens instrument complement on two Quaff B satellites. “Ravens on Quaff” would be a powerful addition to the ILWS program, providing the only global imaging in ILWS, monitoring the IT consequences of disturbances of solar origin, and delivering numerous technical and scientific firsts. 2004/12/09

1.ILWS 2.Ravens Mission Concept 3.Observational Firsts 4.Scientific Firsts 5.Instruments & Heritage 6.Path Forward Ravens on Quaff Talk Outline 2004/12/09

The overarching objective of ILWS is to explore how solar variability affects the Earth environment in the short and long term. ILWS will explore physical processes in the sun-Earth system, focusing on those with planetary-scale effects, and will quantify the geoefficiency of coupling processes. process Source Sink Ravens on Quaff ILWS To accomplish this, we need quantitative observations of the source (such as the solar wind or solar EUV), detailed and comprehensive observations of a geospace process that is of interest, and quantitative observations of sinks (such as the plasmasphere, ionosphere, thermosphere, ring current, & convection) /12/09

Ravens on Quaff ILWS Reconnection, convection, stretching, XX, onset Solar Wind Ring current & CPS energetic particles, Joule heating, & convection Surface waves, fast mode, ULF Pulsations, Wave Particle Interactions Solar Wind Ring Current, Thermosphere, CPS /12/09

EUV Energetic Particles Solar Wind Magnetopause Compression KH/Surface Waves (MPause) Reconnection (MPause) Cusp Entry ULF Waves Drift-Bounce Resonance Wave-Particle Interactions MHD-Scale Instabilities Convection & BBFs Acceleration & Scattering Reconnection (Nightside) Photo-Chemistry Joule Heating Plasmasphere Thermosphere Ionosphere Ring Current Plasma Sheet Radiation Belt process Source Sink Ravens on Quaff ILWS /12/09

 Origin of the plasma sheet  Evolution of the plasma sheet  CPS as a source for the ring current  Energization, transport, & loss of magnetospheric plasma  Magnetospheric instabilities  Storms, superstorms, & the storm-substorm relationship  Midlatitude storm effects  IT response to EUV (detrend magnetospheric input)  Natural complexity (BAS)  Origin of structure in the universe  Magnetic fields in cosmic plasmas Ravens on Quaff Grand Challenge Questions /12/09

Two satellites 180º out of phase in high- inclination high-ellipticity orbits. Each satellite identically instrumented with LBHL & LBHS imagers [U. Calgary Heritage], and a Lyman-α imaging spectrograph [CSL Heritage]. 24 X 7 global auroral imaging. Dedicated modelling and simulation mission component [Robert Rankin]. Other instruments on Quaff B Complement Ravens imaging package Ravens on Quaff Mission Concept /12/09

Ravens on Quaff Mission Concept /12/09

Ravens on Quaff Objectives – Observational Firsts /12/09

Ravens on Quaff Objectives – Observational Firsts /12/09

FUV Auroral Spectrum UVAMC passband LBH bands Lyman-alpha nm nm Ravens on Quaff Objectives – Observational Firsts /12/09

 Simultaneous cross-scale imaging  24 X 7 global auroral imaging  Spectrally resolved global auroral imaging Ravens on Quaff Objectives – Observational Firsts /12/09

 Simultaneous cross-scale imaging  24 X 7 global auroral imaging  Spectrally resolved global auroral imaging  How does auroral structure affect MI coupling?  How does the CPS act as a source for the ring current?  What is the space-time distribution of auroral acceleration mechanisms? Ravens on Quaff Objectives – Observational Firsts Scientific Firsts 11a 2004/12/09

 Simultaneous cross-scale imaging  24 X 7 global auroral imaging  Spectrally resolved global auroral imaging  How does auroral structure affect MI coupling?  How does the CPS act as a source for the ring current?  What is the space-time distribution of auroral acceleration mechanisms? Ravens on Quaff Objectives – Observational Firsts Scientific Firsts 11b 2004/12/09

 Simultaneous cross-scale imaging  24 X 7 global auroral imaging  Spectrally resolved global auroral imaging  How does auroral structure affect MI coupling?  How does the CPS act as a source for the ring current?  What is the space-time distribution of auroral acceleration mechanisms? Ravens on Quaff Objectives – Observational Firsts Scientific Firsts 11c 2004/12/09

 Simultaneous cross-scale imaging  24 X 7 global auroral imaging  Spectrally resolved global auroral imaging  How does auroral structure affect MI coupling?  How does the CPS act as a source for the ring current?  What is the space-time distribution of auroral acceleration mechanisms? Ravens on Quaff Objectives – Observational Firsts Scientific Firsts “Why we need global observations”, by D. J. Williams, in Magnetospheric Physics, Plenum, “Feasibility of a multisatellite investigation of the Earth’s magnetosphere with radio tomography”, by Ergun et al., in JGR, volume 105(A1), pp , d 2004/12/09

: Interball 1: ISIS 2: Viking 3: Feja 5: IMAGE Ravens on Quaff U. Calgary Instrument Heritage 12a 2004/12/09

Ravens on Quaff U. Calgary Instrument Heritage 12b 2004/12/09

Ravens on Quaff U. Calgary Instrument Heritage 12c 2004/12/09

Science RequirementInstrument Parameter Visibility of the auroral oval during daytimeFUV wavelength range Visibility the entire auroral oval 27 deg field of view permits observing the entire oval from 4.4 RE Sufficient spatial resolution to describe the geographic extent of the auroral oval 0.1 degree latitude ~ 100 km Time resolution to describe the global aurora on the scale of substorms 2 minute of faster Sensitivity to observe the baseline quiet time aurora Better than 100 R Measure softness/hardness parameters of electron auroral precipitation based on a known atmospheric model Simultaneous auroral measurement in two spectral regions 24/7 coverage from combined observations of two Ravens vehicles TBD orbit configuration Ravens on Quaff The Path Forward 12d 2004/12/09

Wavelengths: #0 #1 Ravens on Quaff U. Calgary Instrument Heritage 12e 2004/12/09

Miniaturized, low power CCD imaging instrument Optics – three mirror design Dual co-aligned CCD cameras with common DSP controller Low-noise frame transfer CCDs Intensified CCDs Optical axis in spin plane TDI mode Images in LHHs and LBHl Heritage: Viking, Freja, IMAGE, MOST, ePOP Ravens on Quaff U. Calgary Instrument Heritage 12f 2004/12/09

Ravens on Quaff SI-12 – U. Liege/CSL IMAGE Heritage 13a 2004/12/09

Ravens on Quaff SI-12 – U. Liege/CSL IMAGE Heritage 13b 2004/12/09

Ravens on Quaff SI-12 – U. Liege/CSL IMAGE Heritage From Mende et al. [Image FUV Paper I]. 13c 2004/12/09

RoleInternational Partners AISCSL & U. Liege LBHL & LBHSJames Spann Orbital CalculationsJohn Bonnell ??Ground Station, DSP??FMI ??Conjugate Imager??Mark Lester Conjugate SatelliteBrian Fraser ??ENA??Mike Henderson Ravens on Quaff SI-12 – U. Liege/CSL IMAGE Heritage /12/09

Ravens on Quaff Requirements on platform 15a 2004/12/09 ParameterEstimated Allocation Volume Camera #1 Volume Camera # 2 Volume AIS 40 X 20 X 20 cm 3 80 X 50 X 30 cm 3 Volume Electronics Box #1 Volume Electronics Box #2 15 X 15 X 8 cm 3 TBD Mass Camera 1 + Camera 2 Mass AIS 5.5 kg 20.2 kg Power Camera 1 + Camera 2 Power AIS Temperature Range Cameras Temperature Range AIS -10 to 40 celsius (operating) ; -30 to 50 (off) TBD Telemetry Data Rate (total – overestimate)1 Mb/sec pointing accuracy, radiation dose limits, shock tolerance, vibration limits, etc... TBD

Ravens on Quaff Requirements on orbit 15b 2004/12/09

1.Instrument requirements as driven by science objectives (ie., spectrally resolved LBH, spatio-temporal resolution, FOV, cadence, etc). 2.Initial plans for LBHL, LBHS, and AIS. 3.BUS, telemetry, power, orbit, mass requirements as driven by instrument package. 4.Identify Canadian industrial partners (Routes, CAL, etc.). 5.Consider an expanded instrument complement. 6.Clarify the roles of international partners. 7.Develop a comprehensive plan for instrument design, prototyping, building, and payload integration, launch, and operations. 8.Risk assessment & mitigation strategies. 9.Science Plan. Ravens on Quaff The Path Forward 16 DecJanFebMarAprMayJunJulAugSep Orbit Telemetry Mass Power Rough cut to Quaff Final A- to Quaff

 provide the only global imaging in ILWS  deliver >5 technical firsts  deliver significant scientific firsts  place all ILWS & LWS geospace observations in context  motivate significant technological advances  enhance the competitiveness of industry Ravens on Quaff would End 2004/12/09