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: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/mg/mg_9.html
Дата изменения: Thu Sep 15 16:55:02 2005 Дата индексирования: Sat Dec 22 13:59:20 2007 Кодировка: |
The CHIANTI database consists of 4 primary ASCII files for each ion in the database.
contains the energy levels in cm^(-1) It includes both experimental data and theoretical values of the levels energies.
References:
%observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61. %Theoretical energy levels (1-10): Zhang, Sampson, ADNDT, 1992, 52, 143 %theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125. %comment: NIST values for levels 28 (E4) and 31 (F3) are uncertain %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % K.P. Dere, Jan. 1996
contains wavelengths, gf and A values for each transition. Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values.
References:
%observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61 %Theoretical energy levels (1-10): Zhang, Sampson, ADNDT, 1992, 52, 143 %theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125 %A-values: computed using a SSTRUCT model by P.R.Young %comment: A-values computed using a 15 configuration model of the ion. The following configs were included: 2s2, 2s 2p, 2p2 2s 3s, 2s 3p, 2s 3d 2p 3s, 2p 3p, 2p 3d 3s2, 3p2, 3d2 3s 3p, 3s 3d, 3p 3d For the levels with no observed energies, `best-guess' SSTRUCT energies were used, which are more accurate than those derived from the theoretical energies in the .elvlc file. A crucial aspect of this new data is the availability of allowed transitions to de-populate the 3p.3p 3F4 level (level 26) which was previously metastable. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % P.R.Young Jul 1998
contains the spline fits to the electron collision strengths scaled according to Burgess and Tully (1992). Accurate replication of the temperature averaged collision strength over a wide range of temperatures can be accomplished with the data in this file.
References:
%filename: mg_9.splups %oscillator strengths: SUPERSTRUCTURE calculations from P.R> Young (see mg_9.wgfa for details) %effective collision strengths (levels 1 to 10): Keenan et al., Physica Scripta 34, 216, 1986 %collision strengths (levels 11 to 46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125 %comment: the upsilons were calculated in the temperature range 5.2 < Log T < 6.8 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young, Apr 1999
contains the spline fits to the scaled proton collision strengths.
References:
%filename: mg_9.psplups %rates: Ryans R.S.I., Foster-Woods V.J, Copeland F., Keenan F.P., Matthews A., Reid R.H.G., 1998, ADNDT 70, 179-229 %energies: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997 %comment: Fit valid for temp. range 1e5 to 3e7 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 19-Oct-00