| Home | Download | Help | User Guides | Direct access | News - History | Applications |
|---|---|---|---|---|---|---|
| Team | Line Lists | Links | ADS Citations | Acknowledging CHIANTI | CHIANTI papers | CHIANTI and other codes |
The CHIANTI database consists of the following primary ASCII files for this ion:
contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.
%Observed energy levels (1 - 15): Edlen, 1984, Phys.Scripta, 30, 135
%Observed energy levels (16 - 22): Fuhr, J.R., Kelleher, D.E., Martin, W.C., Musgrove, A., Sugar, J., Wiese, W.L.,
Dalton, G.R., Dragoset, R.A., Mohr, P.J., Olsen, K., Reader, J., Saloman, E.B., Sansonetti, C.J.,
Wiersma, G., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%Observed energy levels (n=3): Kink, I, Engstroem, L., 1999, Physica Scripta, 59, 355
%Theoretical energy levels: from the 24-conf model of Bhatia & Landi, 2003, ApJS, 147, 409
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration
%
% E. Landi - Aug 2002
contains wavelengths, gf and A values of the transitions. The wavelengths are based on the experimental energy levels and should be the best available. Wavelengths calculated from the theoretical energies are of an indeterminate accuracy and their values are presented as negative values of the calculated wavelength.
Observed energy levels (1-15): Edlen, 1984, Phys.Scripta, 30, 135
%Observed energy levels (16-22): Fuhr, J.R., Kelleher, D.E., Martin, W.C., Musgrove, A., Sugar, J., Wiese, W.L.,
Dalton, G.R., Dragoset, R.A., Mohr, P.J., Olsen, K., Reader, J., Saloman, E.B., Sansonetti, C.J.,
Wiersma, G., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%Observed energy levels (n=3): Kink, I, Engstroem, L., 1999, Physica Scripta, 59, 355
%A values and oscillator strengths: from the 24-conf model of Bhatia & Landi, 2003, ApJS, 147, 409
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration
%
% E. Landi - Aug 2002
contains the spline fits to the electron collision strengths scaled according the rules formulated by 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.
%filename: s_10.splups
%oscillator strengths (1-15): Zhang, Sampson, 1999, ADNDT, 72, 153
%oscillator strengths (16-22): from the 6-conf model of Bhatia & Landi, 2003, ApJS, 147, 409
%effective collision strengths (levels 1-22): Bell and Ramsbottom, 2000, ADNDT, 76, 176
%Collision strengths (levels 23-72): Bhatia & Landi, 2003, ApJS, 147, 409
%Oscillator strengths (levels 23-72): Bhatia & Landi, 2003, ApJS, 147, 409
%Comment: Corrected errors in the transitions: 1 - 12, 2 - 22, 8 - 22, 12 - 19
%Comment: effective collision strengths are provided in the temperature range 4.6 < Log T < 6.7
%Comment: the effective collision strength at Log T=4.6 of transition 12 - 18 has been omitted from the fit
%Comment: the oscillator strengths have been taken from the 6-configuration calculation for consistency
with the collision strengths
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration
%
% E. Landi and G. Del Zanna - Aug 2002
contains the spline fits to the scaled proton collision strengths.
%filename: s_10.psplups %energies: Bhatia, A.K. Landi, E., 2003, ApJS, 147, 409 %rates: Bhatia, A.K. Landi, E., 2003, ApJS, 147, 409 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - Feb 2003