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Solar Irradiance Observations with LYRA on PROBA2 I. E. Dammasch , M. Dominique, J.-F. Hochedez

Solar Irradiance Observations with LYRA on PROBA2 I. E. Dammasch , M. Dominique, J.-F. Hochedez & the LYRA Team. X th Hvar Astrophysical Colloquium Hvar, Croatia, 6-10 September 2010. LYRA highlights. Royal Observatory of Belgium (Brussels, B)

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Solar Irradiance Observations with LYRA on PROBA2 I. E. Dammasch , M. Dominique, J.-F. Hochedez

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  1. Solar Irradiance Observations with LYRA on PROBA2 I. E. Dammasch, M. Dominique, J.-F. Hochedez & the LYRA Team Xth Hvar Astrophysical Colloquium Hvar, Croatia, 6-10 September 2010

  2. LYRA highlights • 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)…

  3. 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

  4. SWAP and LYRA spectral intervals for solar flares, space weather, and aeronomy LYRA channel 1: the H I 121.6 nm Lyman-alpha line LYRA channel 2: the 200-220 nm Herzberg continuum range LYRA 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

  5. LYRA pre-flight spectral responsivity (filter + detector, twelve combinations)

  6. LYRA data products and manuals… …available at the PROBA2 Science Center: http://proba2.sidc.be/

  7. 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.

  8. 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)

  9. Further Data Products… …“Level 4”, “Level 5” (still preliminary):

  10. State of the data processing pipeline fits fits fits Current state In the future Telemetry packets Not distributed Not distributed LY-TMR: Raw data (in counts) LY-EDG Daily basis After each contact Lv1: Engineering data (in Hz) LY-BSDG fits Not available After each contact Lv2: Calibrated data (in W/m²) Plots + flare list available irregular systematic Other tools Higher level data products

  11. First results (even before opening covers)

  12. Spacecraft maneuvers SAA Aurora Oval • Perturbations appearing around 75° latitude • 2-3 days after a CME, flare ... • Associated to geomagnetic perturbations

  13. First Light acquisition (06 Jan 2010)

  14. Aeronomy • Occultations: Study atmospheric absorption; high temporal resolution needed • Input for atmospheric models: NRT and calibrated data needed

  15. 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

  16. M2.0 flare, 08 Feb 2010, 13:47 UTC

  17. Comparison with GOES flare Example: M1.8 flare, 20 Jan 2010, 10:59 UTC

  18. ComparisonwithGOES flare Example: C5.4 flare, 15 Aug 2010, 18:30 UTC

  19. Sun-Moon eclipse …demonstrating the inhomogeneous distribution of EUV radiation across the solar surface

  20. And we have a fifth channel at 17.4nm... ... called SWAP!

  21. SWAP and LYRA observing together 20100607_proba2_movie.mp4

  22. Next steps • Cross-calibration (internal/external) • Produce calibrated data automatically • Publish first results • Advertise data products • Get extension from ESA

  23. How to be involved? Scientists are welcome to • use PROBA2 data • propose 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 Center • Scientist can take part in the commanding of the instruments • Will gain expertise in the instrumental effects • Next announcement (for 2011-12): May 2011 • Proposal deadline and selection: June 2011 • First visits: September 2011 onwards

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