Difference between revisions of "GOES Flux vs STIX counts"

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[[File:Goes_stix_scatter_polynomial_2oder.png|800px|thumb|none|  Scatter plot of STIX counts (4 - 10 keV) versus GOES flux and  as well as a linear fit and a polynomial fit to the data.  ]]
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[[File:Goes stix flux fit lms.png|800px|thumb|none|  Scatter plot of STIX counts (4 - 10 keV) versus GOES and  as well as a linear fit and a polynomial fit to the data.  ]]
 
The GOES flux of a solar flare is estimated using<br>
 
The GOES flux of a solar flare is estimated using<br>
 
flux=10^(p0+p1*x), <br>
 
flux=10^(p0+p1*x), <br>
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[[File:Goes_background.png |600px|thumb|none|  An example of estimated GOES flux background. ]]
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The scatter plot can be also fitted with a polynomial function.
 
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[[File:Goes stix flux polynomial.png |400px|thumb|none|    A polynomial fit to the data. Occulted flares were excluded. ]]
 
 
 
 
 
[[File:Goes bkg.png |400px|thumb|none|  GOES flux background estimation using algorithm described <a href="https://root.cern.ch/doc/v608/classTSpectrum.html#a56e15d1c36c7557b17d5f6d68fa315a7">here</a> ]]
 

Latest revision as of 10:29, 21 January 2022

Scatter plot of STIX counts (4 - 10 keV) versus GOES and as well as a linear fit and a polynomial fit to the data.

The GOES flux of a solar flare is estimated using
flux=10^(p0+p1*x),
with x=log10(stix_peak_counts*r^2)
where p0, p1 are the parameters from the curve fit, peak_counts is the STIX QL LC peak counts and r is the distance between the Sun and solar orbiter in units of au.


An example of estimated GOES flux background.