1992
DOI: 10.1086/191640
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Abstract: We compute a sequence of five model atmospheres consisting of the photosphere, chromosphere, and transition region. The models represent the response of the gas in a magnetically confined loop to intense flare energy release. We assume that the energy release is confined to the corona, and include the effects of chromospheric evaporation and indirect heating of the lower atmosphere by X-rays emitted from the coronal plasma. The models are computed in hydrostatic and energetic equilibrium and incorporate a deta…

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