Astron. Astrophys. Suppl. Ser. 142, 95-106
Laboratory observation and modeling
of extreme ultraviolet spectra of highly ionized
V.A. Soukhanovskii1 - S. Lippmann2 - M.J. May1 - M. Finkenthal1,5 - H.W. Moos1 - K.B. Fournier3 - W. Goldstein3 - D. Pacella4 - G. Mazzitelli4
Send offprint request: V.A. Soukhanovskii, e-mail: email@example.com
Department of Physics and Astronomy,
The Johns Hopkins University,
Baltimore, Maryland 21218, U.S.A.
2714 Fairview Ave. E. # 101, Seattle, Washington 98102, U.S.A.
Lawrence Livermore National Laboratories,
P.O. Box 808, Livermore, California 94550, U.S.A.
Associazione EURATOM-ENEA sulla Fusione, C.R. Frascati,
CP 65-00044 Frascati Roma, Italy
Permanent address: Racah Institute of Physics, The Hebrew University, Jerusalem, Israel
Received October 8; accepted November 23, 1999
Copyright The European Southern Observatory (ESO)
Benchmarking and validation
of atomic calculations
are crucial for understanding the properties of
astrophysical and fusion plasmas.
An extended re-evaluation of a previous experimental study
of the CaXVIII - CaXII extreme ultraviolet (XUV)
spectra is presented.
into tokamak plasmas and
the spectra of the calcium ions were recorded by
a photometrically calibrated grazing
incidence time-resolved spectrometer.
The local plasma electron
temperature and density were measured independently.
Nearly all features of the line-of-sight
Atomic data for this work were generated ab initio with the
HULLAC suite of codes.
The results of collisional-radiative (CR) modeling
for individual charge states
agree with the measured spectral line intensities
within the experimental accuracy for most lines, thus
validating the electron temperature and density
diagnostic potential of the L-shell lines.
In addition, we compare experimentally measured and calculated
line intensities with those calculated using the CHIANTI
Key words: atomic processes, Sun: UV radiation, Sun: flares