Here we study the inverse problem of obtaining a valid ξ( T) profile from a set of EUV spectral line intensities observed at a pixel within a solar image.Īims. For a prescribed density and temperature structure, it is straightforward to construct the corresponding differential emission measure profile ξ( Τ), such that ξ( Τ) d T is proportional to the emissivity from plasma in the temperature range. Extreme-ultraviolet (EUV) observations provide considerable insight into evolving physical conditions in the active solar atmosphere. Kontar 2ĭepartment of Physics & Astronomy, Western Kentucky University,Į-mail: School of Physics & Astronomy, University of Glasgow,Ĭontext. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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