Abstract
A comparison of Skylab S082A observations for several solar flares with calculations of the electron temperature sensitive emission line ratio R1 = I(2s2p1P − 2s21S)/I(2s2p3P1 - 2s21S) = = I(256.68 A)/I(491.45 A) in Be-like SXIII reveals good agreement between theory and experiment, which provides observational support for the accuracy of the adopted atomic data. However, observed values of the electron density sensitive ratio R2 = I(2s2p1P − 2s21S)/I(2p23P2 - 2s2p3P2) = = I(256.68 A)/I(308.96 A) all lie below the theoretical high density limit, which is probably due to blending in the 308.96 A line.
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