Difference between revisions of "GOES Flux vs STIX counts"

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[[File:Goes-stix-scatter.png|800px|thumb|none| Fig. 1: Scatter plot of STIX counts (4 - 10 keV) versus GOES flux and  histogram of STIX counts versus GOES flux.
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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.  ]]
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STIX counts are background subtracted and divided by the squared distances between Solar Orbiter and the Sun.
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The GOES flux of a solar flare is estimated using<br>
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1045 flares with Earth look-angles smaller than 90 degrees were selected. ]]
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flux=10^(p0+p1*x), <br>
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[[File:Goes-stix-flux-fit.png|600px|thumb|none|  Fig. 2 A profile of the histogram shown in Fig. 1. A cubic function fitted to the profile is also shown. ]]
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with x=log10(stix_peak_counts*r^2)<br>
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where p0, p1 are the parameters from the curve  fit, peak_counts is the STIX QL LC peak
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counts and r is the distance between the Sun and solar orbiter in units of au. <br>
  
  
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The GOES flux of a flare is estimated using<br>
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[[File:Goes_background.png |600px|thumb|none| An example of estimated GOES flux background. ]]
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flux=10^(p0+p1*x+p2**x^2+p3*x^3), <br>
 
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with x=log10(stix_peak_counts)/r^2<br>
 
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where p0, p1, p2 are the parameters from the curve fit, peak_counts is the STIX QL LC peak
 
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counts and r is the distance between the Sun and solar orbiter in units of au.
 
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The error of an estimated flux is considered to be the same as the error of the nearest point, as shown in Fig. 2.
 

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.
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