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Computed vs. Observed Line Profiles of Metallic Atoms in Prominences
Published online by Cambridge University Press: 13 May 2016
Abstract
By solving simultaneously the radiative transfer and statistical equilibrium equations we compute lines profiles for the Ca II H and K lines, Mg II h and k lines and He I at 584,3 Å for several prominence models given by the hydrogen atom. The computed profiles are compared with the observations in order to constrain the physical plasma parameters of solar prominences.
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- Session IV: Structure and Dynamics of the Transiton Region and Corona
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- Copyright © Astronomical Society of the Pacific 2001