Theoretical emission line strengths for the beryllium-like ion Sxiiicompared to XUV observations of solar flares

✍ Scribed by F. P. Keenan; S. M. McCann; K. G. Widing

• Publisher: Springer
• Year: 1988
• Tongue: English
• Weight: 328 KB
• Volume: 117
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00148573

✦ Synopsis

A comparison of Skylab S082A observations for several solar flares with calculations of the electron temperature sensitive emission line ratio R l = I(2s2p lp _ 2s 2 1S)/i(2s2 p 3p1 _ 2s 2 IS) = = 1(256.68 ~)/I(491.45 A,) in Be-like S xnI 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 R 2 = I(2s2p 1p _ 2s 2 1S)/[(2p2 3p2 _ 2s2p 3p2) = = 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.