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Table 4

Ratios of observed and predicted QS line radiances.

λ (Å) 1108 1109 1113 1206 1294.55 1296.73 1298.95+ 1301.15 1303.32 1312.6 1892
1298.89
Skylab (N77) – – – 17.8 0.28 0.20 1.0 0.10 0.34 0.08 23.5
HRTS (N79) – – – – – 0.21 1.0 0.097 – 0.12 –
SUMER 0.25 0.38 0.92 37 0.29 0.22 1.0 – 0.41 0.16 –
log Te[K] = 4.7 0.20 0.52 1.14 18.47 0.28 0.22 1.0 0.12 0.27 0.10 7.8
log Te[K] = 4.65 0.2 0.51 1.12 19.2 0.28 0.22 1.0 0.12 0.27 0.10 8.7
log Te[K] = 4.6 0.18 0.49 1.05 21.51 0.28 0.22 1.0 0.12 0.27 0.08 11.6
log Te[K] = 4.5 0.16 0.43 0.92 29.1 0.28 0.23 1.0 0.13 0.28 0.06 23.2
With QS DEMa 0.18 0.49 1.06 24.8 0.28 0.22 1.0 0.12 0.27 0.09 19.5
With QS DEMb 0.19 0.51 1.12 22.0 0.28 0.22 1.0 0.12 0.27 0.10 14.7
With QS DEMc 0.17 0.46 0.99 29.2 0.28 0.22 1.0 0.12 0.28 0.08 28.8
With QS DEMd 0.18 0.49 1.06 25.7 0.28 0.22 1.0 0.12 0.27 0.09 22.6

Notes. The ratios (in energy units) are relative to the 1298.9 Å self-blend. The Skylab observed ratios are from Nicolas et al. (1977) [N77] and Nicolas et al. (1979) [N79]. (†) The 1312.6 Å measurement is from HRTS. The SUMER measurements are from Pinfield et al. (1999). We then list the predicted ratios with the present atomic data, calculated at four temperatures. The last four rows show the intensity ratios obtained by integration.

(a)

With the DEM obtained by Andretta et al. (2003) (see Appendix) and the CHIANTI v.7.1 ion population (Landi et al. 2013);

(b)

with the DEM obtained from the Skylab QS radiances of Vernazza & Reeves (1978) (see Appendix) and the CHIANTI v.7.1 ion population (Landi et al. 2013);

(c)

with the DEM obtained by Andretta et al. (2003) and the Arnaud & Rothenflug (1985) ion population;

(d)

with the DEM obtained from the Skylab QS radiances of Vernazza & Reeves (1978) and the Arnaud & Rothenflug (1985) ion population.

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