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Solar Irradiance ObservationsSolar Irradiance Observationswith LYRA on PROBA2with LYRA on PROBA2
I. E. Dammasch, M. Dominique, J.-F. HochedezI. E. Dammasch, M. Dominique, J.-F. Hochedez& the LYRA Team& the LYRA Team
Xth Hvar Astrophysical ColloquiumHvar, Croatia, 6-10 September 2010
LYRAthe Large-Yield Radiometer onboard PROBA2
• Royal Observatory of Belgium (Brussels, B)Principal Investigator, overall design, onboard software specification, science operations
• PMOD/WRC (Davos, CH)Lead Co-Investigator, overall design and manufacturing
• Centre Spatial de Liège (B)Lead institute, project management, filters
• IMOMEC (Hasselt, B)Diamond detectors
• Max-Planck-Institut für Sonnensystemforschung (Lindau, D)calibration
• science Co-Is: BISA (Brussels, B), LPC2E (Orléans, F)…
LYRA highlights
LYRA highlights
4 spectral channels covering a wide emission temperature range
Redundancy (3 units) gathering three types of detectors Rad-hard, solar-blind diamond UV sensors (PIN and MSM) AXUV Si photodiodes
2 calibration LEDs per detector (λ = 465 nm and 390 nm) High cadence (up to 100Hz) Quasi-continuous acquisition during mission lifetime
Ly Hz Al Zr
Unit1 MSM PIN MSM Si
Unit2 MSM PIN MSM MSM
Unit3 Si PIN Si Si
SWAP and LYRA spectral intervalsfor solar flares, space weather, and aeronomy
LYRA channel 1: the H I 121.6 nm Lyman-alpha lineLYRA channel 2: the 200-220 nm Herzberg continuum rangeLYRA channel 3: the 17-80 nm Aluminium filter range including the He II 30.4 nm line (+ X-ray)LYRA channel 4: the 6-20 nm Zirconium filter range where solar variablility is highest (+ X-ray)SWAP: the range around 17.4 nm including coronal lines like Fe IX and Fe X
LYRA pre-flight spectral responsivity(filter + detector, twelve combinations)
LYRA data products and manuals…
…available at the PROBA2 Science Center:
http://proba2.sidc.be/
Summary: FITS File Structure
lyra_20100609_000000_lev1_***.fits where: *** = met, std, cal, rej, (bst, bca, bre) generally: header + binary extension table(s) extension = header + data (variable length) Lev1 met = HK, STATUS, VFC Lev1 std = uncalibr. irradiance (counts/ms) Lev2 std = calibr. irradiance (W/m²) Lev3 std = calibr. aver. irradiance (W/m²) per line: time, ch1, ch2, ch3, ch4, qual.
Product Definition
Level 1 = full raw data (LY-EDG output) Level 2 = calibrated physical data (LY-BSDG
output) Caution: preliminary status. Require versioning.
Level 3 = processed products (e.g. averages) Level 4 = plots of products Level 5 = event lists (optionally with plots)
Further Data Products…
…“Level 4”, “Level 5” (still preliminary):
LY-TMR:
State of the data processing pipeline
LY-EDG
LY-BSDG
Telemetry packets
Raw data (in counts)
Lv1: Engineering data (in Hz)
fitsfits
fits
fits
Lv2: Calibrated data (in W/m²)
Other tools Higher level data products
Current state In the future
Not distributed Not distributed
Daily basis After each contact
Not available After each contact
Plots + flare list availableirregular
systematic
First results (even before opening covers)
Aurora Oval
Perturbations appearing around 75° latitude
2-3 days after a CME, flare ...
Associated to geomagnetic perturbations
Spacecraft maneuvers
SAA
First Light acquisition (06 Jan 2010)
Aeronomy
Occultations: Study atmospheric absorption; high temporal resolution needed Input for atmospheric models: NRT and calibrated data needed
Flares
LYRA observes flares down to B1.0
LYRA flare list agrees with GOES14
Flares are visible in the two short-wavelength channels
Exceptionally strong and impulsive flares are also visible in the Lyman- alpha channel (precursor)
Example: C4.0 flare, 06 Feb 2010, 07:04 UTC
M2.0 flare, 08 Feb 2010, 13:47 UTC
Comparison with GOES flare
Example: M1.8 flare, 20 Jan 2010, 10:59 UTC
ComparisonwithGOES flare
Example:C5.4 flare,15 Aug 2010,18:30 UTC
Sun-Moon eclipse
…demonstrating the inhomogeneous distribution of EUV radiation across the solar surface
And we have a fifth channel at 17.4nm...
... called SWAP!
SWAP and LYRA observing together
20100607_proba2_movie.mp4
Next steps
Cross-calibration (internal/external) Produce calibrated data automatically Publish first results Advertise data products Get extension from ESA
How to be involved?
Scientists are welcome touse PROBA2 datapropose special observation campaigns
Guest Investigator Program welcomes proposals for dedicated (joint) observations in the frame of a science project:Funds available for a stay at PROBA2 Science CenterScientist can take part in the commanding of the instrumentsWill gain expertise in the instrumental effects
Next announcement (for 2011-12): May 2011Proposal deadline and selection: June 2011First visits: September 2011 onwards