Stellar and laboratory XUV/EUV line ratios in Fe XVIII and Fe XIX

Journal Article · Fri May 25 00:00:00 EDT 2012 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.4707869· OSTI ID:22004059

Traebert, E; Beiersdorfer, P; Clementson, J ^[1]

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1. Lawrence Livermore National Laboratory, Livermore CA 94550 (United States)

A so-called XUV excess has been suspected with the relative fluxes of Fe XVIII and Fe XIX lines observed in the XUV and EUV ranges of the spectrum of the star Capella as observed by the Chandra spacecraft, even after correction for interstellar absorption. This excess becomes apparent in the comparison of the observations with simulations of stellar spectra obtained using collisional-radiative models that employ, for example, the Atomic Plasma Emission Code (APEC) or the Flexible Atomic Code (FAC). We have addressed this problem by laboratory studies using the Livermore electron beam ion trap (EBIT).

• OSTI ID: 22004059
• Journal Information: AIP Conference Proceedings, Vol. 1438, Issue 1; Conference: 17. international conference on atomic processes in plasmas (ICAPIP), Belfast, Northern Ireland (United Kingdom), 19-22 Jul 2011; Other Information: (c) 2012 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

70 PLASMA PHYSICS AND FUSION TECHNOLOGY
79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTRONOMY
ASTROPHYSICS
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
CORRECTIONS
COSMIC PHOTONS
ELECTRON BEAMS
EXTREME ULTRAVIOLET RADIATION
IRON IONS
MULTICHARGED IONS
PLASMA
PLASMA DIAGNOSTICS
PLASMA SIMULATION
STARS
STELLAR RADIATION
TRAPS