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First Results from the LYRA Solar UV Radiometer J.-F. Hochedez , I. E. Dammasch , M. Dominique

First Results from the LYRA Solar UV Radiometer J.-F. Hochedez , I. E. Dammasch , M. Dominique & the LYRA Team. COSPAR 38 th Scientific Assembly Bremen 18-25 July 2010 8 th Annual TIGER Symposium. LYRA highlights. Royal Observatory of Belgium (Brussels, B)

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First Results from the LYRA Solar UV Radiometer J.-F. Hochedez , I. E. Dammasch , M. Dominique

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  1. First Results from the LYRA Solar UV Radiometer J.-F. Hochedez, I. E. Dammasch, M. Dominique & the LYRA Team COSPAR 38th Scientific Assembly Bremen 18-25 July 2010 8th Annual TIGER Symposium

  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. First results (even before opening covers)

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

  9. First Light acquisition (06 Jan 2010)

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

  11. 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

  12. M2.0 flare, 28 Feb 2010, 13:47 UTC

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

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

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

  16. SWAP and LYRA observing together 20100607_proba2_movie.mp4

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