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 versus GOES flux | + | [[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. |
| − | STIX counts are divided by the squared distances between Solar Orbiter and the Sun. 1045 flares with look-angles | + | STIX counts are background subtracted and divided by the squared distances between Solar Orbiter and the Sun. |
| − | [[File:Goes-stix-flux-fit.png|600px|thumb|none| Fig. 2 A profile of the histogram shown in Fig. 1. A cubic function | + | 1045 flares with Earth look-angles smaller than 90 degrees were selected. ]] |
| + | [[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. ]] | ||
Revision as of 08:45, 18 January 2022
File:Goes-stix-flux-fit.png
Fig. 2 A profile of the histogram shown in Fig. 1. A cubic function fitted to the profile is also shown.
The GOES flux of a flare is estimated using
flux=10^(p0+p1*x+p2**x^2+p3*x^3),
with x=log10(stix_peak_counts)/r^2
where p0, p1, p2 are the parameters from the polynomial 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.
