Table 4
Integrated intensities of the He ii 256 Å line and the blending lines in different regions of the corona (C) and the prominence (P).
| Integrated Intensity/Box | P-7 | P-8 | P-9 | C-6 | C-10 | LY(obser) | LY (pred) | Y (obser) |
|
|
||||||||
| Total emission | 323 | 353 | 328 | 224 | 191 | 176 | ||
| He ii | 50 | 40 | 37 | |||||
| coronal blends | 135 | 125 | 138 | 174 | 151 | 157 | 139 | |
| Si x 256.37 | 92 | 85 | 94 | 101 | 95 | |||
| 1/2 (Si x 256.37) | 46 | 42 | 47 | |||||
| Si x 261.04 | 104 | 90 | 84 | |||||
|
|
||||||||
| Fe xii 195.12 | 520 | 482 | 534 | 681 | 575 | 581 | 761 | |
|
|
||||||||
| He ii (model 1) | 143 | 183 | 145 | |||||
| He ii (model 2) | 189 | 225 | 192 | |||||
| He ii (model 3) | 165 | 205 | 167 | |||||
| He ii (model 4) | 211 | 247 | 214 | |||||
Notes. The total emission quoted here is corrected for the background emission, which is assumed to be of instrumental origin. LY refers to the paper of Landi & Young (2010) and to CHIANTI computations by E. Landi (private communication), (obser) to observed values, (pred) to predicted values, Y to Young’s EISWiki. We note that LY values correspond to a height in the corona of about 25 000 km, which is somewhat lower than in the present work.
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