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GOES M9 Flare 20 October 2012 18:05 18:14 18:19 UT AR 11598

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 20 October 2012 18:05 18:14 18:19 UT AR 11598

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  1. GOES M9 Flare20 October 2012 18:05 18:14 18:19 UT AR 11598 Brian Dennis 24 October 2012

  2. GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT

  3. 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.

  4. GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT vth + thin2 Fe abundance = 4.95 x coronal!!!

  5. GOES M9 FlareAR 11598, 20 October 2012 18:05 18:14 18:19 UT vth + thin2 Fe abundance = 0.6 x coronal Systematic residuals

  6. 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

  7. 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

  8. 22 Oct. 2012 18:11:52 to 18:12:20 UT12 to 25 keV MEM-NJIT CLEAN

  9. GOES X2 Flare23 October 2012 AR 11598 Brian Dennis 24 October 2012

  10. 23 October 2012

  11. 23 October 2012

  12. 23 October 2012

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