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SPHINX DATA ANALYSIS

SPHINX DATA ANALYSIS. Magdalena Gryciuk. Astronomical Institute, University of Wroclaw Space Research Centre, Polish Academy of Sciences. I SOLARNET SPRING SCHOOL, WROCŁAW, 28.03.2014 . Outline. SPHINX INSTRUMENT SPHINX OBSERVATIONS SPHINX & GOES SMALL EVENTS CATALOGUE

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SPHINX DATA ANALYSIS

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  1. SPHINX DATA ANALYSIS Magdalena Gryciuk Astronomical Institute, University of Wroclaw Space Research Centre, Polish Academy of Sciences I SOLARNET SPRING SCHOOL, WROCŁAW, 28.03.2014

  2. Outline • SPHINX INSTRUMENT • SPHINX OBSERVATIONS • SPHINX & GOES • SMALL EVENTS CATALOGUE • SCIENCE WITH SPHINX

  3. SphinX:SolarPhotometerinX-ray CORONAS - Photon SphinX SphinXmission

  4. SphinXMissionObservations, 2009 Countrate [count/s] Flux [W/m2] GOES 3.726e-09 W/m2 3.7 S • SphinX level1 data catalogue • - The catalog contains data from D1 SphinXdetector • All available data files are stored in FITS format • (OGIP-93/003 format) NEW SXR FLARES CLASSES S CLASS - S1 = 1. e-09 W/m2 Q CLASS - Q1 = 1. e-10 W/m2 http://156.17.94.1/sphinx_l1_catalogue/SphinX_cat_main.html

  5. SphinX & GOES observations GOES threshold = 3.726e-09 W/m2 3.7 S D1 minimum = ~2.e-10 W/m22.0 Q GOES Threshold

  6. SphinXEvents List - automatic detection algorithm Algorithm step by step: 1. Data preparation: Resampling and averaging of SphinX light curve (optimal: 70s) 2. Searching for continuous increase of 4 consecutive points and 3 continuous decreases points after them 3. Finding times of maxima between increasing and decreasing series of points 4. Visual inspection and corrections EVENT LIST STEP BY STEP: 1. Data preparation: Resampling and averaging of SphinX light curve (optimal: 70s) 2. Searching for continuous increase of 4 consecutive points and 3 continuous decreases points after them 3. Finding times of maxima between increasing and decreasing series of points 4. Visual inspection and corrections Algorithm have detected 1431 FLARES Log count/s

  7. FlaresCharacteristics Flareafterbackgroundsubtraction Tstart time of start Tendtime of end Tmax time of maximum Flaremagnitude TstartTmaxTend Flaremagnitude Optimalfitting Linearbackground fbackg(t) = E t + F 1% abovethebackgroundlevel

  8. ElementarySoft X-ray FlareProfile Convolution of twofunctions Gauss function Exponentialfunction * FLARE PROFILE FORMULA: Linearscale Log scale Linearbackground 4 parameters (flare) + 2 parameters (linearbackground-attributable) = 6 PARAMETERS

  9. SimpleFlaresObserved by SphinX 26 May 2009 A 1.01

  10. SimpleFlaresObserved by SphinX 04 June 2009 A 8.40

  11. SimpleFlaresObserved by SphinX 07 July 2009 A 9.95

  12. BlendedFlares 05 June 2009

  13. SphinXCatalogue - FuturePlans • Work on SphinXflaring events catalogue: FLARE ID , Timestart , Timemax , Timeend , Flaremagnitude • Extended catalogue (Temperatures, Fluxes, …) • Flarecharacteristicsanalysis • Analysis of flarefluxobservation in 1-8 Å wavelengthrange

  14. The following research areas, in which SphinX measurements may find application, have been identified: • Analysis of the Sun as a star • Investigation of quiet-Sun soft X-ray flux • Observations of active regions • Identification of small solar events and analysis of their energetics and statistical properties • Space weather and climate • Characterization of the particle environment in the CORONAS–PHOTON orbit • Determination of coronal plasma physical parameters • Search for transient and non-Maxwellian processes in solar plasma • Comparison of soft X-ray flux and TSI variability • Cross-comparison with other X-ray spectrometers • Verification of the abundance and ionization equilibrium models used in solar spectroscopy

  15. ThankYou

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