Post on 30-Dec-2015
description
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
RavensThe “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. ILWS2. Ravens Mission Concept3. Observational Firsts4. Scientific Firsts5. Instruments & Heritage6. 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.
processSource 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).
1 2004/12/09
Ravens on Quaff ILWS
Reconnection,convection, stretching,XX, onset
SolarWind
Ring current & CPSenergetic particles,
Joule heating, &convection
Surface waves,fast mode,
ULF Pulsations,Wave Particle Interactions
SolarWind
Ring Current,Thermosphere,
CPS
2 2004/12/09
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
processSource Sink
Ravens on Quaff ILWS
3 2004/12/09
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
4 2004/12/09
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
5 2004/12/09
Ravens on Quaff Mission Concept
200420052006
6 2004/12/09
Ravens on Quaff Objectives – Observational Firsts
7 2004/12/09
Ravens on Quaff Objectives – Observational Firsts
8 2004/12/09
FUV Auroral Spectrum
UVAMC passband
LBH bands
Lyman-alpha
135.6 nm
130.4 nm
Ravens on Quaff Objectives – Observational Firsts
9 2004/12/09
Simultaneous cross-scale imaging 24 X 7 global auroral imaging Spectrally resolved global auroral
imaging
Ravens on Quaff Objectives – Observational Firsts
10 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
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
11c2004/12/09
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, 1990.
“Feasibility of a multisatellite investigation of the Earth’s magnetosphere with radio tomography”, by Ergun et al., in JGR, volume 105(A1), pp 361-373, 2000.
11d 2004/12/09
1971 1986 1986
1996 2000
4: Interball
1: ISIS2: Viking3: 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 Requirement Instrument Parameter
Visibility of the auroral oval during daytime FUV 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
Role International Partners
AIS CSL & U. Liege
LBHL & LBHS James Spann
Orbital Calculations John Bonnell
??Ground Station, DSP?? FMI
??Conjugate Imager?? Mark Lester
Conjugate Satellite Brian Fraser
??ENA?? Mike Henderson
Ravens on Quaff SI-12 – U. Liege/CSL IMAGE Heritage
14 2004/12/09
Ravens on Quaff Requirements on platform
15a 2004/12/09
Parameter Estimated AllocationVolume Camera #1
Volume Camera # 2
Volume AIS
40 X 20 X 20 cm3
40 X 20 X 20 cm3
80 X 50 X 30 cm3
Volume Electronics Box #1
Volume Electronics Box #2
15 X 15 X 8 cm3
TBD
Mass Camera 1 + Camera 2
Mass AIS
5.5 kg
20.2 kg
Power Camera 1 + Camera 2
Power AIS
<4 W>
<4.4 W>
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
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
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Dec Jan Feb Mar Apr May Jun Jul Aug Sep
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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...
17 - End2004/12/09