goes m9 flare 20 october 2012 18 05 18 14 18 19 ut ar 11598
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GOES M9 Flare 20 October 2012 18:05 18:14 18:19 UT AR 11598. Brian Dennis 24 October 2012. GOES M9 Flare AR 11598, 20 October 2012 18:05 18:14 18:19 UT. GOES M9 Flare AR 11598, 20 October 2012 18:05 18:14 18:19 UT. Detectors #1 and 6 have finest energy resolution.

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goes m9 flare ar 11598 20 october 2012 18 05 18 14 18 19 ut
GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT
  • Detectors #1 and 6 have finest energy resolution.
  • Fe line complex at 6.7 keV
  • “Background” lines at ~8 and ~11 keV.
goes m9 flare ar 11598 20 october 2012 18 05 18 14 18 19 ut1
GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT

vth + thin2

Fe abundance

= 4.95 x coronal!!!

goes m9 flare ar 11598 20 october 2012 18 05 18 14 18 19 ut2
GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT

vth + thin2

Fe abundance

= 0.6 x coronal

Systematic residuals

goes m9 flare ar 11598 20 october 2012 18 05 18 14 18 19 ut3
GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT

multitherm_abun_pow+ thin2

Fe abundance

= 0.6 x coronal

Reduced chi-squared

= 0.91

conclusions
Conclusions
  • Detectors 1, 3, 6, 7, 8, 9 are working well.
  • Detector 6 has remarkably good energy resolution.
  • Detector 3 has lower sensitivity as always
  • Use visibility normalization to determine relative detector sensitivities –
    • 1.03,0.00,1.11,0.00,1.01,1.06,0.94,0.92,0.96
goes x2 flare 23 october 2012 ar 11598

GOES X2 Flare23 October 2012 AR 11598

Brian Dennis

24 October 2012

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