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

16

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