Abstract
Recent calculations of atomic data for Fe XV have been used to generate theoretical line ratios involving n = 3–4 transitions in the soft X‐ray spectral region (∼52–83 A) for a wide range of electron temperatures and densities applicable to solar and stellar coronal plasmas. The line ratio calculations are compared with solar flare observations from a rocket‐borne spectrograph (XSST) and with a co‐added spectra of Capella obtained with the Chandra LETGS, representing the highest signal‐to‐noise observation achieved for a stellar source in the 30–80 A soft X‐ray region. Results are promising for use of Fe XV as astrophysical plasma diagnostics: Agreement between theory and observation is generally good, after particular account is taken of line blending. The 82.76 A emission line in the XSST spectrum is identified, for the first time to our knowledge in an astrophysical source, as the 3s3d 3D3−3s4p 3P2 transition of Fe XV.
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