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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 20 october 2012 18 05 18 14 18 19 ut ar 11598

GOES M9 Flare20 October 2012 18:05 18:14 18:19 UT AR 11598

Brian Dennis

24 October 2012


GOES M9 FlareAR 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
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


22 oct 2012 18 11 52 to 18 12 20 ut 12 to 25 kev
22 Oct. 2012 18:11:52 to 18:12:20 UT12 to 25 keV

MEM-NJIT

CLEAN


Goes x2 flare 23 october 2012 ar 11598

GOES X2 Flare23 October 2012 AR 11598

Brian Dennis

24 October 2012





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