Table 3
Ratios of the intensities of transition region to coronal lines measured on the prominence and in the corona.
| Line | H1 | H2 | ||
| I(P2)/I(C1) | I(P4)/I(C5) | I(P7)/I(C6) | I(P9)/I(C10) | |
|
|
||||
| Increase of TR emission | ||||
| Fe viii 185.21 | 1.07 | 2.34 | 1.34 | 2.33 |
| Fe viii 186.60 | 1.09 | 2.34 | 1.21 | 2.37 |
| Si vii 275.35 | 1.07 | 2.19 | 1.24 | 2.67 |
|
|
||||
| Decrease of coronal emission | ||||
| Fe xii 195.12 (r) | 0.63 | 0.88 | 0.76 | 0.93 |
| XRT (rb) | 0.74 | 0.94 | 0.85 | 1.00 |
|
|
||||
| τ195 (α = 0.5) | 0.33 | 0.14 | 0.22 | 0.15 |
| τ195 (α = 0.3) | 0.62 | 0.24 | 0.39 | 0.27 |
Notes. rb is the ratio of coronal emission at a position in the prominence to a position outside in XRT data. The optical thickness at 195 Å is derived by assuming a spherically symmetric corona with the prominence lying in the plane of the sky (α = 0.5) and for an asymmetric corona where the prominence lies behind the plane of the sky (α = 0.3).
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