Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..774..349d&link_type=abstract
X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: Theory, Experiment, and Observation. AIP Conference Proceedings, Volume 774, pp. 34
Astronomy and Astrophysics
Astrophysics
Stellar Atmospheres, Solar Corona, Astrophysical Plasma, X-Ray Sources (Astronomical), Plasma Diagnostics, X-Ray Spectra, Magnetohydrodynamics And Plasmas, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, X-Ray, X-Ray And Gamma-Ray Measurements
Scientific paper
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 Å) 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 Å 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 Å 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.
Aggarwal Kanti M.
Bloomfield Shaun D.
Brickhouse Nancy S.
Chung Sungki
Drake Jeremy J.
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