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

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 SRC-PAS early experiments Sounding rocket experiment XRT telescope on Hinode satellite

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

8. GOES 12, Mass 2T, Mid 1970's – present, Orbit geostationary 35,790 km 1m

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

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

12. RECENT SRC-PAS EXPERIMENTS RESIKSphinXRF-15I

13. 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

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

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

17. RF-15I photometer/imager, INTERBALL – Tail spacecraft August 1995 – December 1997 30 cm energy range 2 - 240 keV proportional detectors Gas Ar+10%CO 2, 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

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

19. 10 cm RF-15I detectors Calibration source

20. 2 – 3 keV 3 – 5 keV 5 – 8 keV 10 – 15 keV 15 – 30 keV 30 - 60 keV Time UT, 2 February 1997 Counts per second RF-15I example of data

21. 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 % CO 2. Resolution ~ 10 m Å. The wavelength coverage, 3.3 Å - 6.1 Å, includes emission lines of Si, S, Cl, Ar, and K Four wavelength channels Printed in Zaragoza 02 July 2013 RESIK Bragg-cristal spectrometer CORONAS-F satellite August 2000 – May 2003

22. RESIK detectors 10 cm

23. RESIK example spectra

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

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