Difference between revisions of "GOES Flux vs STIX counts"
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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 stix flux polynomial.png |400px|thumb|none| A polynomial fit to the data. Occulted flares were excluded. ]] | ||
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| + | [[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> ]] | ||
Revision as of 20:22, 20 January 2022
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.
GOES flux background estimation using algorithm described <a href="https://root.cern.ch/doc/v608/classTSpectrum.html#a56e15d1c36c7557b17d5f6d68fa315a7">here</a>
