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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 (1-6): Feldman et al, 2000, ApJ, 544, 508 %Observed energy levels (6-15): Edlen, 1984, Phys.Scripta, 30, 135 %Observed energy levels (3d: 52,56,57,58,62,63,67,68,70,74): J.R. Fuhr, D.E. Kelleher, W.C. Martin, A. Musgrove, J. Sugar, W.L. Wiese, G.R. Dalton, R.A. Dragoset, P.J. Mohr, K. Olsen, J. Reader, E.B. Saloman, C.J. Sansonetti, G. Wiersma, "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data %Observed energy levels (3s: 17,18,20): Kaufman, V., Sugar, J., Cooper, D., 1982, Phys. Scr., 26, 163 %Theoretical energy levels: Bhatia & Landi 2005, ADNDT, in press %comment: theoretical energy levels come from the 24-configuration calculation in Bhatia & Landi (2005) % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Enrico Landi - April 2004
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 (1-6): Feldman et al, 2000, ApJ, 544, 508 %Observed energy levels (6-15): Edlen, 1984, Phys.Scripta, 30, 135 %Observed energy levels (3d: 52,56,57,58,62,63,67,68,70,74): J.R. Fuhr, D.E. Kelleher, W.C. Martin, A. Musgrove, J. Sugar, W.L. Wiese, G.R. Dalton, R.A. Dragoset, P.J. Mohr, K. Olsen, J. Reader, E.B. Saloman, C.J. Sansonetti, G. Wiersma, "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data %Observed energy levels (3s: 17,18,20): Kaufman, V., Sugar, J., Cooper, D., 1982, Phys. Scr., 26, 163 %Theoretical energy levels: 24-conf. model from Bhatia & Landi 2005, ADNDT, in press %A values and oscillator strengths: Bhatia & Landi 2005, ADNDT, in press %comment: theoretical energy levels and all radiative data come from the 24-configuration calculation in Bhatia & Landi (2005) % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Enrico Landi - April 2004
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: ca_14.splups %Collision strengths: Landi & Bhatia, 2005, ADNDT, in press %Oscillator strengths: Landi & Bhatia, 2005, ADNDT, in press %comment: oscillator strengths have been taken from the 6-configuration model of Bhatia & Landi (2005) for consistency with the collisional calculation % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - Apr 2004