The intensity ratio variation of the Si IV 1394/1403 Å lines during solar flares - Resonance scattering and opacity effects

Open Access

Fig. 7.

Time evolution of the height distribution of the contribution function at the line core (top panel), the population ratio n₂/n₁ (middle panel), and the proportion of the resonance scattering to thermal emission X (bottom panel) for Case f10E15d3. An obvious enhancement of the contribution function in the chromosphere starts from t = 5.0 s.

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