Topical Issue - Space Weather Instrumentation
Open Access
Technical Article

Table 1

Strong lines in the COSIE-S wavelength range.

Ion and wavelength (Å) Log maximum temperature Expected signal (ph s−1)
QS AR Flare
O v 192.91 5.35 0.7 3.6 2120
O ivi 184.12 5.45 0.6 7.4 500
Fe viii 185.21 5.65 10.9 102 4460
Fe ix 188.50 5.85 10.1 104 1760
Fe x 184.54 6.05 18.8 234 2800
Fe xi 188.22 6.15 30.4 577 6570
Fe xii 195.12 6.20 30.8 1135 14,355
Fe xii 186.88 6.20a 8.7 304 3800
Fe xiii 202.04 6.25 5.8 548 8620
Fe xiii 203.83 6.25a 4.0 355 5520
S xi 191.27 6.30 0.5 50 960
Ar xiv 194.39 6.55 0.0 8.1 1130
Ca xiv 193.87 6.55 0.0 20.6 3500
Ca xv 200.97 6.65 0.0 13.6 4840
Ca xvii 192.86 6.75 0.0 26.2 62,200
Fe xxiv 192.04 7.25 0.0 0.0 80,690
a

Density-sensitive line.

The final three columns give the signal in the COSIE-S channel for three standard Chianti differential emission measures, assuming a density of 109 cm−3, under quiet sun, active region, and flare conditions folded through the COSIE-S effective area. Intensities are calculated using the solid angle associated with a COSIE-S pixel and integrated over the spectral line.

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