J/A+AS/125/149 CHIANTI - An Atomic Database For Emission Lines I. (Dere+ 1997)
CHIANTI - an atomic database for emission lines.
I. Wavelengths greater than 50 Angstroms
Dere K.P., Landi E., Mason H.E., Monsignori Fossi B.C., Young P.R.
<Astron. Astrophys. Suppl. Ser. 125, 149 (1997)>
=1997A&AS..125..149D 1997A&AS..125..149D (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics
Keywords: atomic data - astronomical data bases: miscellaneous -
ultraviolet: general - Sun: atmosphere - stars: atmosphere
Abstract:
A comprehensive set of accurate atomic data is required for analyses
of astrophysical and solar spectra. CHIANTI provides a database of
atomic energy levels, wavelengths, radiative data and electron
excitation data for ions which are abundant in cosmic plasmas. The
most recent electron excitation data have been assessed and stored
following the method of Burgess & Tully (1992A&A...254..436B 1992A&A...254..436B). The
current version is essentially complete for specifying the emission
spectrum at wavelengths greater than 50Å. A list of observed lines
in the spectral region between 50 and 1100Å has been compiled and
compared with the lines predicted by the CHIANTI database. The CHIANTI
database reproduces the vast majority of lines observed at these
wavelengths. CHIANTI includes IDL (Interactive Data Language) routines
to calculate optically thin synthetic spectra for equilibrium
conditions. IDL routines to calculate theoretical line intensities
required for electron density or temperature diagnostics and emission
measure studies are also included. The CHIANTI atomic database and
supporting IDL routines are available by anonymous FTP.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3 96 1768 A list of observed lines and lines in the
CHIANTI database between 50 and 1100 Angstroms
table3.tex 137 2020 LaTeX version of table3
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See also:
J/A+A/370/1071 : Fe XII UV line intensity ratios (Binello+, 2001)
http://wwwsolar.nrl.navy.mil/chianti.html : CHIANTI homepage
Byte-by-byte Description of file: table3
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm LamObs Observed wavelength from literature sources (1)
10- 17 F8.3 0.1nm LamCH ? Wavelength in CHIANTI database
20- 27 A8 --- Ion Ion (spectroscopic notation)
29- 46 A18 --- Level1 Description of lower level of transition
48 A1 --- --- [-] Separation dash
50- 75 A26 --- Level2 Description of upper level of transition
77- 83 E7.2 mW/m2/sr Int ? Predicted intensity of line in a small
solar flare (2)
86- 94 A9 --- Ref Literature sources of observed wavelength (3)
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Note (1): The observed wavelength is given as 0. if there is not report of an
observed line at the wavelength of a reasonably intense line
predicted by CHIANTI
Note (2): The intensity is given a 0. if the line is identified but is not
included in the CHIANTI database.
Note (3): References:
1: Acton et al. (1985ApJ...291..865A 1985ApJ...291..865A)
2: Behring et al. (1972ApJ...175..493B 1972ApJ...175..493B)
3: Behring et al. (1976ApJ...203..521B 1976ApJ...203..521B)
4: Dere (1978ApJ...221.1062D 1978ApJ...221.1062D)
5: Freeman & Jones (1970SPh....15..288F 1970SPh....15..288F)
6: Thomas & Neupert (1994, Cat. J/ApJS/91/461)
7: Widing & Sandlin (1968ApJ...152..545W 1968ApJ...152..545W)
8: Kastner et al. (1974ApJ...191..261K 1974ApJ...191..261K)
9: Burton & Ridgeley (1970SPh....14....3B 1970SPh....14....3B)
10: Feldman & Doschek (1991ApJS...75..925F 1991ApJS...75..925F)
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Acknowledgements: Ken Dere
References:
Young et al., CHIANTI. II 1998A&A...329..291Y 1998A&A...329..291Y
Landi et al., CHIANTI. III 1999A&AS..135..339L 1999A&AS..135..339L
(End) Patricia Bauer [CDS] 22-Apr-1997