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

SPHINX INSTRUMENT SPHINX INSTRUMENT SPHINX OBSERVATIONS SPHINX OBSERVATIONS SPHINX & GOES SPHINX & GOES SMALL EVENTS CATALOGUE SMALL EVENTS CATALOGUE SCIENCE WITH SPHINX SCIENCE WITH SPHINX Outline

SphinX BASIC INFORMATIONS LAUNCHED:30 January 2009 at 13:30 UT from Plesetsk Cosmodrom SATELLITE:CORONAS – Photon ORBITS PARAMETERS: orbit duration- 96 min altitude - 550km near polar orbit MASS:3.7 kg POWER:10 W ENERGY RANGE:1.2 keV - 15 keV in 256 energy bins LIFESPAN OF THE MISSION: 20 February - 29 November 2009 SphinX:Solar Photometer in X-ray SphinX: Solar Photometer in X-raySphinX CORONAS - Photon SphinX mission

Count rate [count/s] SphinX Mission Observations, NEW SXR FLARES CLASSES S CLASS - S1 = 1. e-09 W/m 2 S CLASS - S1 = 1. e-09 W/m 2 Q CLASS - Q1 = 1. e-10 W/m 2 Q CLASS - Q1 = 1. e-10 W/m 2 NEW SXR FLARES CLASSES S CLASS - S1 = 1. e-09 W/m 2 S CLASS - S1 = 1. e-09 W/m 2 Q CLASS - Q1 = 1. e-10 W/m 2 Q CLASS - Q1 = 1. e-10 W/m 2 Flux [W/m 2 ] GOES 3.726e-09 W/m S SphinX level1 data catalogue - The catalog contains data from D1 SphinX detector - All available data files are stored in FITS format (OGIP-93/003 format) (OGIP-93/003 format)

SphinX & GOES observations GOES Threshold GOES threshold = 3.726e-09 W/m S D1 minimum = ~2.e-10 W/m Q

SphinX Events List - automatic detection algorithm 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 Log count/s 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 Algorithm have detected 1431 FLARES

Flares Characteristics T start time of start T end time of end T max time of maximum Flare magnitude 1% above the background level Linear background f backg (t) = E t + F T max T start T max T end Flare magnitude Optimal fitting Flare after background subtraction

Convolution of two functions Gauss function Exponential function Elementary Soft X-ray Flare Profile Linear background FLARE PROFILE FORMULA: * 4 parameters (flare) + 2 parameters (linear background- attributable) = 6 PARAMETERS Linear scale Log scale

Simple Flares Observed by SphinX 26 May 2009 A :34:0410:44:4711:06:42 Time start Time max Time end

Simple Flares Observed by SphinX 04 June 2009 A :56:1018:00:5618:21:12 Time start Time max Time end

Simple Flares Observed by SphinX 07 July 2009 A :06:4310:08:3810:22:08 Time start Time max Time end

Blended Flares 05 June 2009

Work on SphinX flaring events catalogue: Work on SphinX flaring events catalogue: FLARE ID, Time start, Time max, Time end, Flare magnitude FLARE ID, Time start, Time max, Time end, Flare magnitude Extended catalogue (Temperatures, Fluxes, …) Extended catalogue (Temperatures, Fluxes, …) Flare characteristics analysis Flare characteristics analysis Analysis of flare flux observation in 1-8 Å wavelength range Analysis of flare flux observation in 1-8 Å wavelength range SphinX Catalogue - Future Plans

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

Thank You