LAGRANGE REMOTE SENSING INSTRUMENTS: THE EXTREME ULTRAVIOLET IMAGER (EUVI)
C. Kintziger (CSL) - Presenter
S. Habraken (CSL)
P. Bouchez (CSL)
Matthew West (ROB)
David Berghmans (ROB)
Manfred Gyo (PMOD/WRC)
Margit Haberreiter (PMOD/WRC)
Jackie Davies (RAL Space)
Martin Caldwell (RAL Space)
Ian Tosh (RAL Space)
Stefan Kraft (ESA)
1 ESWW 2018, 9 Nov. 2018
LGRRS-EUVI | Mission overview
2 ESWW 2018, 9 Nov. 2018
See Poster 23 by J. Davies 4 remote-sensing instruments
LGRRS-EUVI | Mission overview
3 ESWW 2018, 9 Nov. 2018
5 in-situ instruments
LGRRS-EUVI | Mission overview
4 ESWW 2018, 9 Nov. 2018
• Overall Remote Sensing Instruments leader: RAL Space (UK)
• EUVI study led by three institutes:
– CSL (BE)
– ROB (BE)
– PMOD/WRC (CH)
• CSL activities
– EUVI Instrument manager:
• Overall management
• System study
• Optical engineering
• Thermal engineering
• AIT engineering
• Roles & Responsibilities
– BPI: Pr. Dr. Serge Habraken (CSL)
– Bco-I: Dr. Matthew J West (ROB)
– CSL work funded by Belspo via Prodex Programme
• ROB activities
– instrument requirements
– instrument operation
– ground segments
• PMOD activities
– electrical engineering
– mechanisms
– mechanical engineering
LGRRS-EUVI | Mission overview
5 ESWW 2018, 9 Nov. 2018
Parameter Requirement
Spectral resolution < 1.5 𝑛𝑚 𝐹𝑊𝐻𝑀
Spatial resolution < 5 𝑎𝑟𝑐𝑠𝑒𝑐
Field of view 42.6′ 𝑥 42.6′
Mass < 8 𝑘𝑔
Size < 600 𝑥 150 𝑥 150 𝑚𝑚
Power < 10 𝑊
• EUV Imager
– SSA programme (SWE)
– Location: L5
– Goal: image the full solar disc
– Waveband: EUV wavelength (e.g. 193 Å)
– Heritage: PROBA-2 SWAP
ESIO (GSTP)
Solar Orbiter EUI
LGRRS-EUVI | Instrument overview
6 ESWW 2018, 9 Nov. 2018
Semi-Static Structures Filaments/Prominences Active Regions Coronal Holes
Dynamic structures Flares Eruptions EUV Waves Dimmings
Regions Chromosphere Million Degree Corona
131 nm 19.5 nm 30.4 nm
• Selected wavelengths
LGRRS-EUVI | Instrument overview
7 ESWW 2018, 9 Nov. 2018
• Field of view
– Differs between selected wavebands
1. 195 Å
2. 131 + 304 Å
Toward Earth
62 arcmin
43 arcmin
43 arcmin
43 arcmin
LGRRS-EUVI | Instrument overview
8 ESWW 2018, 9 Nov. 2018
Channel 1
Channel 2
EUVI Optical Unit
Detector
Detector
PE
PE
Entrance f ilter
Entrance f ilterFEE DC/DC
Power
HK, data
Door
TC
EUVI Electronic Box
Filter wheel
Door
FPA camera
Mechanism
control
Optical sy stem
Optical sy stem
FPA camera
IPU
• Detector: EUI spare 3k by 3k, separate windowing options
1. 195 Å: 2300x1600, 1,6”/pixel, 3.2” spat. res. over 2 pixels
2. 131 + 304 Å: 2x2 binning, 800x800, 3.2”/pixel, 6.4” spat. res. over 2 pixels
• Cadence: Different for each spectral channel
1. 195 Å: 3 min
2. 131 Å: 2 min
3. 304 Å: 5 min
• Schematic configuration:
LGRRS-EUVI | Instrument overview
9 ESWW 2018, 9 Nov. 2018
• Obtained design
– ESIO-like truss structure
• Separate avionic box
• Lightweight and stiff
– SWAP-based optical design
• Improved spatial resolution and larger
FOV wrt SWAP (and ESIO)
• Similar baffling system
– Filter wheel
• Selects between 131 and 304 observation
– One-shot opening doors
LGRRS-EUVI | Performed analyses
10 ESWW 2018, 9 Nov. 2018
• Performed analyses
– Understanding of requirements
– Optical design
• Tolerancing
• Straylight
– Electrical design
– Instrument performance model
– Thermal analysis:
• Undergoing at CSL
– Structural analysis
• Undergoing at PMOD/WRC
EUVI Electronics
Electronic Box
IPCU
Optical Unit
Camera 1 SpW 2*(1)
SpW 2*(1)
Power 2*(1)
Heater EB 2*(1)
Filter Wheel Power
Power
Camera 2
EB HK Control
EB HK Control
EUVI-A CCSDS SpW 2*(1)
Thermistor EB 2*(1)
EUVI-B CCSDS SpW 2*(1)
EUVI SU 2*(1)
Radiator Thermal LinkHeater TL 2*(1)
Thermistor TL 2*(1)
Heater APS(A) 2*(1)
Thermistor APS(A) 2*(1)
Heater APS(B) 2*(1)
Thermistor APS(B) 2*(1)
EUVI Survival Heater RadiatorLink
EUVI Thermistor RadiatorLink
EUVI Operational Heater APS (A)
EUVI Thermistor APS (A)
EUVI Operational Heater APS (B)
EUVI Thermistor APS (B)
EUVI Survival Heater EB
EUVI Thermistor EB
LGRRS-EUVI | Performed analyses
• Encountered issues:
– Coating: dual-band coating for 131 + 304 Å is not “off-the-shelf” because those two
wavelengths do not fall within two successive Bragg orders (need to be factor ~2
between wavelengths)
• is feasible
• requires simulation and development
Other alternatives:
• Superpose 2 mono-band coatings on top of each other
• Implement a patterned coating on primary mirror
will lead to ~50% loss in efficiency BUT mono-band coating may be as
high as 2x more efficient than dual-band.
11 ESWW 2018, 9 Nov. 2018
LGRRS-EUVI | Way forward after PRR
12 ESWW 2018, 9 Nov. 2018
LGRRS-EUVI | Conclusion
13 ESWW 2018, 9 Nov. 2018
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