Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/ti/ti_16.html
Дата изменения: Thu Sep 15 16:56:47 2005 Дата индексирования: Sat Dec 22 14:04:01 2007 Кодировка: Поисковые слова: south pole |
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 (1 - 15): Edlen, 1984, Phys.Scripta, 30, 135 %Observed energy levels (n=3): Fuhr et al 1999, NIST Database for Atomic Spectroscopy, Version 2.0, NIST Standard Reference Database # 78 %Theoretical energy levels (1 - 15): Zhang, Sampson, ADNDT, 1999, 72, 153 %Theoretical energy levels (16 - 72): Bhatia, A.K., Seely, J.F., Feldman, U., 1989, ADNDT 43,99 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna, May 2001.
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:
%Experimental energy levels (1 - 15): Edlen, 1984, Phys.Scripta, 30, 135 %Experimental energy levels (16 - 72): NIST Database for Atomic Spectroscopy, Version 2.0, 1999, NIST Standard Reference Database # 78 %Theoretical energy levels (16 - 72): Bhatia, A.K., Seely, J.F., Feldman, U., 1989, ADNDT 43, 99 %A values for transitions indicated within the ground configuration: Merkelis et al., 1999, Physica Scripta 59, 122 %A values for allowed n=2 transitions: Zhang, Sampson, ADNDT, 1999, 72, 153 %A values for non-allowed n=2 transitions: Merkelis et al., 1999, Physica Scripta 59, 122 %A and gf values for transitions from n=3 levels (16-72): Bhatia, A.K., Seely, J.F., Feldman, U., 1989, ADNDT 43, 99 %gf values for transitions between the (1 - 15) levels: Zhang, Sampson, ADNDT, 1999, 72, 153 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna, Jan 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: ti_16.splups %oscillator strengths (levels 1 - 15): Zhang, Sampson, 1999, ADNDT, 72, 153 %%oscillator strengths (levels 16 - 72): Bhatia,A.K., Seely,J.F., Feldman,U., 1989, ADNDT, 43, 99 %collision strengths (levels 1 - 15): Zhang, Sampson, 1999, ADNDT, 72, 153 %collision strengths (levels 16 - 72 only from the ground): Bhatia,A.K., Seely,J.F., Feldman,U., 1989, ADNDT, 43, 99 %comment: the original collision strengths for levels 16 - 72 were calculated only at one single energy. % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna, May 2001
contains the spline fits to the scaled proton collision strengths.
References:
%filename: ti_16.psplups %rates: Bhatia, A.K., Feldman, U., Doschek, G.A., 1980, J. Appl. Phys. 51, 1464 %energies: Bhatia, A.K., Feldman, U., Doschek, G.A., 1980, J. Appl. Phys. 51, 1464 %comment: Fitted using single_temp.pro with scalx=0.90 %comment: The authors did not give data for the 4-5 transition. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 16-May-01