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Space Research Centre Polish Academy of Sciences, SRC-PAS Solar Physics Division

Solar space-born instruments and detectors for X-ray observations of the solar corona. Szymon Gburek. Space Research Centre Polish Academy of Sciences, SRC-PAS Solar Physics Division 51-622 Wrocław, Kopernika 11 MPGD 2013/RD51, 1 – 6 July, 2013, Zaragoza, Spain. OUTLINE.

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Space Research Centre Polish Academy of Sciences, SRC-PAS Solar Physics Division

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  1. Solar space-born instruments and detectors for X-ray observations of the solar corona.Szymon Gburek Space Research Centre Polish Academy of Sciences, SRC-PAS Solar Physics Division 51-622 Wrocław, Kopernika 11 MPGD 2013/RD51, 1 – 6 July, 2013, Zaragoza, Spain

  2. OUTLINE • About the group(SRC-PAS) • Solar X-ray observation • SRC-PAS solar experiments

  3. SPACE RESEARCH CENTER POLISH ACADEMY OF SCIENCES WARSAW SOLAR PHYSICS DIVISION WROCLAW

  4. SOLAR PHYSICS DIVISION, SRC PAS – WROCLAW the website http://www.cbk.pan.wroc.pl/ http://www.cbk.pan.wroc.pl/?l=EN&act=1 English

  5. WHY STUDY THE SUN IN X-RAYS Solar corona is well seen in short wavelength radiation – studies of coronal heating problem Studies of triggering, evolution and spectroscopy of solar flares - the most energetic events in the Solar System. Determining coronal plasma physical parameters T, EM Improving models of solar chemical composition – element abundances Tstin plasma ionisation equlibrium Space weather

  6. Past and present solar soft X-ray imaging XRT telescope on Hinode satellite SRC-PAS early experiments Sounding rocket experiment

  7. Overwiev of solar activity as seen by GOES satellites 1 – 8 Angstrom wavelength range

  8. Solar spectra – theory – generated with CHIANTI code Big flare Active Sun Quiet Sun http://www.chiantidatabase.org/

  9. Quiet 15 September 2009 Active 14 November 2012 Solar limb Large solar flare 13May 2013

  10. RECENT SRC-PAS EXPERIMENTS RF-15I RESIK SphinX

  11. 20 cm Solid state detectors Si – PIN diodes Energy range ~1 - 15 keV Resolution ~0.4 keV SphinX: Solar Photometer in X-rays CORONAS – Photon satellite February – November 2009

  12. X-RAYS D1 D2 D3 SphinX detectors and optics AMPTEK Si PIN-DIODES XR-100CR X-RAYS Al entrance filters Be detector windows Seven orders of magnitude of solar X-ray flux covered

  13. SphinX GOES-10 SphinX/GOES-10 X-ray measurements in 2009

  14. 30 cm energy range 2 - 240 keV proportional detectors Gas Ar+10%CO2, 350 Torr 2 - 3, 3 - 5, 5 - 8 keV scintillation detector NaI(Tl) crystal 10-15, 15-30, 30-60, 60-120, 120-240 keV RF-15I photometer/imager, INTERBALL – Tail spacecraft August 1995 – December 1997

  15. Imager assembly photometer assembly RF-15I instrument, top view, no cover.

  16. RF-15I detectors Calibration source 10 cm

  17. RF-15I example of data 2 – 3 keV 3 – 5 keV 5 – 8 keV Counts per second 10 – 15 keV 15 – 30 keV 30 - 60 keV Time UT, 2 February 1997

  18. Figure 3: Left: RF15-I soft X-ray Photometer-Imager flown on INTERBALL-Tail mission. Center: Imager assembly of RF15-I, Right image obtained from RF15-I (grid is 50×50 arcsec). Gas equal xenon - argon mixture with 5 % CO2. Resolution ~10mÅ. The wavelength coverage, 3.3 Å - 6.1 Å, includes emission lines of Si, S, Cl, Ar, and K Four wavelength channels RESIK Bragg-cristal spectrometer CORONAS-F satellite August 2000 – May 2003 Printed in Zaragoza 02 July 2013

  19. RESIK detectors 10 cm

  20. RESIK example spectra

  21. Further SRC-PAS satellite projects Development of the next solar X-ray Bragg – crystal spectrometer Development of a solar X-ray polarimeter

  22. Thank you More in the posters and another talk tomorrow!!!

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