|
Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/ni/ni_15.html
Дата изменения: Thu Sep 15 16:58:28 2005 Дата индексирования: Sat Dec 22 14:03:46 2007 Кодировка: Поисковые слова: п п п п п п п п п п п п п п п п п п п п 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:
%energy levels(1-4,7-9,15,23): Sugar & Corliss, 1985, J.Phys.Chem.Ref.Data, 14, Suppl.2 %energy levels(18-20,22,24-26): Sugar, Kaufman & Rowan, 1992, J.Opt.Soc.America B %energy levels(5,12,13): Kelly, 1987, J.Phys.Chem.Ref.Data, 16, Suppl.1 %theoretical energy levels: Mason (unpublished) %comment: The third set of energies were deduced from the radiative data obtained by "superstructure". These energies are not directly from superstructure, but are "corrected" by an amount suggested by comparing a superstructure model of Fe XIII with the observed energies of Fe XIII (all 27 levels are accurately known for Fe XIII). We estimate that the energies so obtained are accurate to +/- 2000 cm-1. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % P.R.Young and E.Landi 1999
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(1-4,7-9,15,23): Sugar & Corliss, 1985, J.Phys.Chem.Ref.Data, 14, Suppl.2
%observed energy levels(18-20,22,24-26): Sugar, Kaufman & Rowan, 1992, J.Opt.Soc.America B
%observed energy levels(5,12,13): Kelly, 1987, J.Phys.Chem.Ref.Data, 16, Suppl.1
%A values: obtained from `superstructure' using a 35 configuration model
%Comment: the following configurations were included:
3s2 {3p2, 3p3d, 3d2, 3p4s, 3p4p, 3p4d, 3p4f, 3d4s, 3d4p, 3d4d, 3d4f}
3s2 {3p5s, 3p5p, 3p5d, 3p5f, 4p4d, 4p2}
3s3p2 {3d, 4s, 4p, 4d, 4f}
3p3 {3d, 4s, 4p, 4d, 4f}
3s3d3, 3p23d2, 3s3p3, 3s3p3d2
3p4, 4p4, 3s4p3, 3p3d3
%comment: as with Fe XIII, level 17 is metastable and magnetic quadrupole
transitions down to the ground are important.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% P.R.Young and E.Landi 1999
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: ni_15.splups
%collision and oscillator strengths: H.E. Mason (unpublished)
%comment: a 4 configuration target was used in Mason's calculation, with
3s2 3p2, 3s 3p3, 3s2 3p 3d, 3p4
Collision strengths are only tabulated for the first 3 configurations.
The gf values given above were obtained by running a 4 configuration
model on `superstructure'. The allowed transition gf values were
within 5% of those of Mason.
As the collision strengths were only tabulated for one energy, two
types of fitting were used: for allowed transitions the high energy
limit point created an extra point, allowing a straight line fit.
For all other transitions, the high energy limit point was set to
zero, which forces the physically realistic situation of the
collision strength tending to zero at infinity.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% P.R. Young - 1995
contains the spline fits to the scaled proton collision strengths.
References:
%file: ni_15.psplups %rates: Faucher, P. 1977, A&A 54, 589 %energies: Faucher, P. 1977, A&A 54, 589 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 13-Dec-2001