Comparison of Fe XVIII and Fe XIX Line Emissions with Spectral Models

Details Comparison of Fe XVIII and Fe XIX Line Emissions with Spectral Models Comparison of Fe XVIII and Fe XIX Line Emissions with Spectral Models

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..774..155d&link_type=abstract

X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: Theory, Experiment, and Observation. AIP Conference Proceedings, Volume 774, pp. 15

Astronomy and Astrophysics

Astrophysics

1

X-Ray Spectra, X-Ray Sources (Astronomical), Atomic Structure, Atomic Collisions, Stars, X-Ray Spectra, Atomic And Molecular Data, Spectra, And Spectral Parameters, Atomic Processes And Interactions, X-Ray

Scientific paper

We discuss here the observations of Fe XVIII and XIX emission lines and compare the X-ray, EUV and FUV lines with the spectral codes widely used today (e.g. FAC and APEC). We assess the relative accuracy of these spectral models and try to identify the critical atomic data and processes. Capella with a narrow enhancement in its emission measure distribution at 6 MK provides a unique opportunity to test the Fe XVIII and Fe XIX model emissivities which peak from 6 to 8 MK. We use the summed spectra from Chandra HETG/ACIS-S and LETG/HRC-S, as well as contemporaneous EUVE and FUSE observations, to measure line ratios for comparison with predictions.

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