Abstract
The standard two-level picture of Lyα thermalization does not formally apply in the solar case because at temperatures typical for Lyα formation (T ≥ 15000 K), the collisional rate from level 2 to level 3 greatly exceeds the collisional rate from level 2 to level 1. For electron densities typical of quiescent solar line formation, this collisional interlocking is not a significant consideration owing to the greater importance of radiative interlocking effects. However, when strong flare heating enhances the free electron density to the order of 10 13 cm −3 , it is found that the important collisional rate from level 2 to level 3 supports an upward series of collisions leading ultimately to the continuum
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