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: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/fe/fe_24.html
Дата изменения: Thu Sep 15 16:54:46 2005 Дата индексирования: Sat Dec 22 14:03:27 2007 Кодировка: Поисковые слова: apollo 11 |
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 (1-24): Del Zanna, 2005, A&A, in press %Theoretical energy levels (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %observed energy levels (above ionization: 25,26,29,30,32,36,38-40): Shirai,T. et al., 2000, J.Phys.Chem.Ref.Data, Monograph 8 %Theoretical energy levels (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2003, A&A, 403, 339 %comment: theoretical energies for levels 27,28,31,33-35,37 have been used as experimental energies %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and E. Landi - Jun 27, 2005
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 (1-24): Del Zanna, 2005, A&A, in press %Theoretical energy levels (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %observed energy levels (25,26,29,30,32,36,38-40): Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8 %Theoretical energy levels (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2003, A&A, 403, 339 %comment: theoretical energies for levels 27,28,31,33-35,37 have been used as experimental energies %Radiative data (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %Radiative data (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and E. Landi - Jun 27, 2005
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: fe_24.splups %Oscillator strengths (1-15): Berrington and Tully 1997, A&AS, 126, 105 %Oscillator strengths (16-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %gf values (above ionization): Palmeri, P., Mendoza, C., Kallman, T.R., Bautista, M.A., 2003, A&A, 403, 1175 %Effective collision strengths (1-15): Berrington and Tully 1997, A&AS, 126, 105 %Effective collision strengths (16-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 %comment: rate coefficients are to be considered valid in the 1.6x10^6 -- 10^8 K temperature range. %comment: Only the excitations from the first 3 levels are retained here. These are sufficient up to high (10^{19} cm-3) electron densities, since these are the levels mostly populated %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and E. Landi - Jun 27, 2005