Kapustin Yar Sounding rockets 7 launches 1970 1971 1977 1979 1980 1981 1983 1984

1. Past politicalopportunities: Intercosmos1967no launchpaymentshttp://www.cbk.pan.wroc.pl/body/publikacje/2005/PTA_Solar_htm.html Plesetsk Orbital missions 3 launches 1994 Coronas-I 1995 Interball-Tail 2001 Coronas-F Kapustin Yar Sounding rockets 7 launches 1970 1971 1977 1979 1980 1981 1983 1984

2. The First Polish Space experiment Pin-hole cameras

3. The Team: PI Janusz Sylwester SphinX soft X-ray spectrophotometer • Mirek Kowalinski : Project Manager • Jarek Bakała: Project Constructor • Szymon Gburek: Project Scientist • Marek Siarkowski, Barbara Sylwester, • Zbigniew Kordylewski, Piotr Podgórski, • Witold Trzebiński, Stefan Płocieniak, Anna Kępa • FIAN: Dr. Sergey Kuzin, TESIS PI • MEPhI: YuryKotov, CORONAS-Photon PM • AI CzAS: Dr. Franta Farnik • Prof. Fabio Reale, INAFA, Palermo University Prof. Ken Phillips, UCL, London http://www.cbk.pan.wroc.pl/body/publikacje/2008/SphinX.pdf

4. CORONAS-F launch, orbit & pointing 31 July 2001, polar orbit, 95min, ~500 km semi-Sun-synchronous SS-14 Cyclone x 10, CORONAS-F http://coronas.izmiran.rssi.ru/F/instruments

5. Satellite CORONAS-PHOTON TESIS SphinX STEP-F KONUS-RF-anti pressure vessel PHOKA RT-2/GA RT-2/S KONUS-RF N-2M RT-2/G PINGUIN Magnetometer Launch is fixed to the last week of 2008 !

7. Full Solar disk UV & soft X-ray monitors

8. TESIS assembly of instrumentsfor XUV imaging spectroscopy of the Sun It is advanced version of the SPIRIT instrument http://www.tesis.lebedev.ru/

9. SphinX & TESIS TESIS SphinX

10. Instruments for charge particle measurements 3-axis magnetometer

11. SphinX construction • EUV filters (doublyaluminizedMylar) • Photometer • Collimators(+-2.5 deg) • Threeapertures • D1, D2, D3 • Shutter • Stepper motor • FFU • Filters • Targets • D4 • Electronics • Front endAmptek • Digital „our” • Controller • Software • reprogramming • Heatsink • Alignment mirror

12. Measurement channels P h o t o m e t r i c FFU D2 D1 D3 D4 φ: 5 mm A: 13.0 mm2 8 μs Up to 60 000 cts/s FWHM: 490 eV φ: 4 mm A: 0.26 mm2 25 μs Up to 20 000 cts/s FWHM: 290 eV φ: 4 mm A: 0.0052 mm2 25 μs Up to 20 000 cts/s FWHM: 290 eV φ: 4 mm A: 13.0 mm2 25 μs Up to 20 000 cts/s FWHM: 290 eV $4000 Detectors (four units): 256/1024energy bins Amptek, Peltier cooled (-50 deg) Si PIN diodes. Detectors’ support plate thermally connected to external heat radiator via heat sink pipe. Photon arrival time measured towithin 2μs(in Time Stamping Mode) Much better energy resolution than gas detectors 2.5 %against16%, low thermal noise http://www.carroll-ramsey.com/detect.htm

13. Expected total count rates Courtesy; Marek Siarkowski

14. SphinX calibration BESSY synchrotron Berlin February 26th 2008 March 2nd 2008 D3 RAS Meeting 9 May 2008 Janusz Sylwester, Poland: Ongoing and future solar X-ray experimenting

15. How it looks from the tests The BESSY synchrotron input spectrum (red) with overplotted response of SphinX D2 detector (black). Nominal effective areas have been used. The agreement is better than 5% in the energy band where SphinX detectors are the most sensitive. BESSY Berlin Synchrotron: - All detector linearity: perfect (0.1% ) over 0.8-14.5 keV; dynamic range 104. - absolute response known to better than 5% against reference synchrotron source. - pile-up matrices known as measured fromX-ray 4 crystal monochromator spectra obtained at 8 energies between 1.5 and 8 keV

16. The measurement environment, bcgd: ~few cts/s up to 103 cts/s (SAA) SAA Night RB RB Night Flare CORONAS-F • Important pahases • S/C X-ray day • S/C optical day • S/C optical night • S/C X-ray night • Terminator crossing Previous CORONAS-F orbit

17. Time stamping mode D1, D2 or D3 rates < 103/s • Time stampingmodefrom: D1, D2, D3, D4 • 2 Bytes for processor time of thedetectorevent start • 1 byte for theamplitude • Allows to determinethedifferencebetweenevents to within 2 μs ~2/1000 accuracy • Absolute timing to within 0.001s against UT Expectedrates D1= 103events/s (event: Amplitude 1byte, time 2 bytes)-3 KB/s D2= 10 events/s, D3= 10 events/s, D4= 10 events/s Total: 3Kbytes/s – canlast for ~10000s (3 h) eachdump – maycover 100% cyclewithcompression

18. Waiting time analysis – is the process at low count rate Poissonian?Wheatland, The Astrophysical Journal, Volume 679, Issue 2, pp. 1621-1628, 2008 • Radioactivesourcesgive an idealexample of thestatistics • To whatdegreethearrivaltimes of photonsfromthe „quiet” coronahave „no memory” i.etheyhavetheexponentialwaiting time distribution? (Modelsfor flare statistics assume or predict that flares are independent events- howeverthisis under question) • Theprimarytask for theinitial part of themissionwheretheactivityisexpected to be low.

19. SphinX convolved spectra (Acoronal) O, Ne,Fe Shape depends on T Si Ca Ar Fe S Ni Fe Ni 25 MK pure continuum 10 MK 5 MK

20. Predicted behaviour of activity during active phase of Coronas-Photon http://science.nasa.gov/headlines/y2006/10may_longrange.htm

21. Recent GOES & RHESSI

22. Energy Calibration • D1,D2,D3 solar induced fluorescence spectra of pure elements • During flares ~> M1 • Until 10^6 cts collected for each detector • Approximately each month • If v. quiet condition then on the command from the ground for 10 min

23. Terminator transit: Profile of Earth atmospecric absorption • X-ray terminator crossing algorithm operational on board • Predict the entry/exit to within few seconds • Spectra 256 energy bins each 0.1 sec give at least 1 km resolution in the vertical Earth absorption profile • Time stamping or spectral mode depending on the flare flag

24. SphinX firstshttp://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The_SphinX_Instrument_on_CORONAS-PHOTON • SphinX will measure absolute element abundances using line features due to neon, magnesium, silicon, sulphur, argon, calcium, iron and nickel in various levels of solar activity (quiet Sun, active regions and flares). It should therefore be in a strong position to give a definitive answer to the continuing debate about the dependence of coronal abundances of elements on their first ionization potential, the so-called FIP effect. • SphinX will obtain the first absolutely calibrated solar X-ray spectra in the 0.8--15 keV range. In particular this will help us to understand the RHESSI continuum observations in this difficult range. • SphinX will also study quiet coronal heating processes via photon arrival time--distance analysis (the arrival time of an X-ray photon will be measured to a couple of microseconds); X-ray oscillations in the <1 to 500 s period range; and transient ionization in flares.

25. Instrument satus • Flight model at the Moscow „factory” undergoing final electro-magnetic & teelmetry compatibility tests • On November 30, TESIS ( a mother instrument for SphinX) is coming for a final maintenance tests to FIAN (MK+WT) will reload the flight programme • The Coronas-Photon launch is expected before the end of 2008 a X-mas present? • Ground sector of software v1 ready (Czech contribution under guidance od Szymon) • 2 mirror servers (Wrocław, Ondrejov) • Automatic data access to FIAN SphinX data stream (~12 hours maximum delay if 2 dumps/24h) • Automatic reduction to Level2 • Data publishing to the public access area (90% data will go there decision taken by the duty scientist) • Automatic flare event catalogue creation start,max, end, class, Tmax, Emmax, rise phase dur L, H, EMmax-Tmax delay • Auxiliary data available: GOES, RHESSI, SOXS

26. The FFU unit (filter-fluorescence unit) Filter-Fluorescence Unit (FFU) layout This unit will be active all the time: time stamping < 1000 cts/s or spectra (256 bins)