sphinx data analysis magdalena gryciuk astronomical institute, university of wroclaw space research...
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SPHINX DATA ANALYSIS
Magdalena Gryciuk
Astronomical Institute, University of WroclawSpace Research Centre, Polish Academy of Sciences
I SOLARNET SPRING SCHOOL, WROCŁAW, 28.03.2014
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• SPHINX INSTRUMENT• SPHINX OBSERVATIONS• SPHINX & GOES• SMALL EVENTS CATALOGUE• SCIENCE WITH SPHINX
Outline
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SphinX BASIC INFORMATIONS
LAUNCHED: 30 January 2009 at 13:30 UT from Plesetsk Cosmodrom
SATELLITE: CORONAS – Photon
ORBITS PARAMETERS:
orbit duration- 96minaltitude - 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
CORONAS - Photon
SphinX mission
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Coun
t rat
e [c
ount
/s]
SphinX Mission Observations, 2009
http://156.17.94.1/sphinx_l1_catalogue/SphinX_cat_main.html
NEW SXR FLARES CLASSES S CLASS - S1 = 1. e-09 W/m2 Q CLASS - Q1 = 1. e-10 W/m2
Flux
[W/m
2 ]
GOES 3.726e-09 W/m2 3.7 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)
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SphinX & GOES observations
GOES Threshold
GOES threshold = 3.726e-09 W/m2 3.7 SD1 minimum = ~2.e-10 W/m2 2.0 Q
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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 them3. Finding times of maxima between increasing and decreasing series of points4. Visual inspection and corrections
Log
cou
nt/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 them3. Finding times of maxima between increasing and decreasing series of points4. Visual inspection and corrections
Algorithm have detected 1431 FLARES
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Flares CharacteristicsTstart time of start
Tend time of end
Tmax time of maximum
Flare magnitude
1% above the background level
Linear backgroundfbackg (t) = E t + F
Tstart Tmax Tend
Flare magnitude
Optimal fitting
Flare after background subtraction
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Convolution of two functionsGauss function
Exponential function
Elementary Soft X-ray Flare Profile
Linear background
)/)(( 22
)( CBtAetf
)()( Dtetf
FEttfbg )(
FLARE PROFILE FORMULA: *
4 parameters (flare) +2 parameters (linear background-attributable) = 6 PARAMETERS
Linear scale Log scale
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Simple Flares Observed by SphinX
26 May 2009A 1.01
10:34:04 10:44:47 11:06:42
Timestart Timemax Timeend
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Simple Flares Observed by SphinX
04 June 2009A 8.40
17:56:10 18:00:56 18:21:12
Timestart Timemax Timeend
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Simple Flares Observed by SphinX
07 July 2009A 9.95
10:06:43 10:08:38 10:22:08
Timestart Timemax Timeend
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Blended Flares
05 June2009
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• Work on SphinX flaring events catalogue: FLARE ID , Timestart , Timemax , Timeend , Flare magnitude• Extended catalogue (Temperatures, Fluxes, …)• Flare characteristics analysis• Analysis of flare flux observation in 1-8 Å wavelength range
SphinX Catalogue - Future Plans
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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
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Thank You