Magdalena Gryciuk Astronomical Institute University of Wroclaw Space Research Centre Polish Academy of Sciences I SOLARNET SPRING SCHOOL WROCŁAW 28032014 SPHINX INSTRUMENT SPHINX ID: 249546
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Slide1
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 Slide2
SPHINX INSTRUMENT
SPHINX
OBSERVATIONS
SPHINX & GOES
SMALL EVENTS CATALOGUESCIENCE WITH SPHINX
OutlineSlide3
SphinX
BASIC INFORMATIONS
LAUNCHED:
30 January 2009 at 13:30 UT from Plesetsk CosmodromSATELLITE: 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 binsLIFESPAN OF THE MISSION: 20 February - 29 November 2009
SphinX
:
Solar Photometer in X-ray
SphinX
CORONAS - Photon
SphinX
missionSlide4
Count
rate [count/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/m
2 Q CLASS - Q1 = 1. e-10 W/m2
F
lux
[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)Slide5
SphinX
& GOES
observations
GOES Threshold
GOES threshold = 3.726e-09 W/m
2 3.7 SD1 minimum
= ~2.e-10 W/m2
2.0 QSlide6
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 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
FLARESSlide7
Flares
Characteristics
T
start time of start
Tend
time of end
Tmax
time of
maximum
Flare
magnitude
1%
above the background level
Linear
background
fbackg (t) = E t + F
Tstart Tmax
Tend
Flare magnitude
Optimal
fitting
Flare
after
background
subtractionSlide8
Convolution
of
two
functions
Gauss
function
Exponential
function
Elementary
S
oft
X-ray
Flare
Profile
Linear
background
FLARE PROFILE FORMULA:
*
4
parameters
(
flare
) +
2
parameters
(
linear
background-attributable
) = 6 PARAMETERS
Linear
scale
Log
scaleSlide9
S
imple
Flares
Observed by
SphinX
26 May 2009
A 1.01
10:34:04
10:44:47
11:06:42
Time
start
Time
max
Time
endSlide10
S
imple
Flares
Observed by
SphinX
04
June
2009
A 8.40
17:56:10
18:00:56
18:21:12
Time
start
Time
max
Time
endSlide11
S
imple
Flares
Observed by
SphinX
07
July
2009
A 9.95
10:06:43
10:08:38
10:22:08
Time
start
Time
max
Time
endSlide12
Blended
Flares
05
June
2009Slide13
Work
on
SphinX
flaring events catalogue: FLARE ID ,
Time
start ,
Time
max ,
Timeend
,
Flare
magnitude
Extended
catalogue
(Temperatures, Fluxes, …)Flare
characteristics
analysis
Analysis
of flare flux observation in 1-8 Å wavelength rangeSphinX
Catalogue - Future
PlansSlide14
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 spec
troscopySlide15
Thank
You