|
Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/si/si_7.html
Дата изменения: Thu Sep 15 16:57:19 2005 Дата индексирования: Sat Dec 22 13:59:39 2007 Кодировка: Поисковые слова: п п п п п п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п |
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 (n=2): Fuhr, J.R., et al., "NIST Atomic Spectra Database" ver. 2.0
March 1999. NIST Physical Reference Data
%observed energy levels (12,19,23-26,65-67,69,70,72-74,78-82,84,85): Fuhr, J.R., et al.,
"NIST Atomic Spectra Database" ver. 2.0 March 1999. NIST Physical Reference Data
%observed energy levels (16-18,20,21,29,31-34,40-42,46,48,52,55,57,59,62,63): Kink, I., Jupen, C.,
Engstroem, L., Feldman, U., Laming, J.M., Schuehle, U., 1997, ApJ, 487, 956
%observed energy levels (11,13-15,22,28,30,35-37,43-45,47,49-51,53,54,56,60,61,64,68,71,75-77,86):
Kink, I., Engstroem, L., 1997, Physica Scripta, 56, 31
%theoretical energy levels: From the 24-configuration model by Bhatia, A.K., Landi, E., 2003, ApJ, 585, 587
% Comment: The observed energy of level 11 is in reality theoretical. It has been inserted so that
energies of levels 16,17,18 could be determined from its value and the experimental
energy difference measured by Kink et al 1997 from transitions involving each of these levels
with level 11. The energy of levels 40,41,42 has then been determined from the energy difference
measured by Kink et al 1997 for the transitions between levels 16-18 and 40-42.
This means that the absolute energies of levels 16,17,18,40,41,42 are probably offset by
a constant value, but their energy difference is experimentally correct. This allows
CHIANTI to correctly calculate the transition wavelengths from these levels, to reproduce
lines observed by SUMER in solar active and quiet spectra.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Oct 2002
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 (n=2): Fuhr, J.R., et al., "NIST Atomic Spectra Database" ver. 2.0
March 1999. NIST Physical Reference Data
%observed energy levels (12,19,23-26,65-67,69,70,72-74,78-82,84,85): Fuhr, J.R., et al.,
"NIST Atomic Spectra Database" ver. 2.0 March 1999. NIST Physical Reference Data
%observed energy levels (16-18,20,21,29,31-34,40-42,46,48,52,55,57,59,62,63): Kink, I., Jupen, C.,
Engstroem, L., Feldman, U., Laming, J.M., Schuehle, U., 1997, ApJ, 487, 956
%observed energy levels (11,13-15,22,28,30,35-37,43-45,47,49-51,53,54,56,60,61,64,68,71,75-77,86):
Kink, I., Engstroem, L., 1997, Physica Scripta, 56, 31
%theoretical energy levels: From the 24-configuration model by Bhatia, A.K., Landi, E., 2003, ApJ, 585, 587
%Radiative data: From the 24-configuration model by Bhatia, A.K., Landi, E., 2003, ApJ, 585, 587
%Radiative data transition within the ground configuration: Tachiev, G.I., Froese Fischer, C., 2002, A&A, 385, 716
%Radiative data 3-4 and 4-5 transitions: Froese Fischer, C., Saha, H.P., 1983, Phys. Rev. A., 28, 3169
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Oct 2002
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: si_7.splups %oscillator strengths: Bhatia, A.K., Landi, E., 2003, ApJ, 585, 587 %collision strengths: Bhatia, A.K., Landi, E., 2003, ApJ, 585, 587 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - Oct 2002
contains the spline fits to the scaled proton collision strengths.
References:
%file: si_7.psplups %rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished. %energies: Observed values, from .elvlc file %comment: Fits valid for temperatures 1.75e5 to 6e6 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 15-May-2001