Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://www.arcetri.astro.it/science/chianti/chianti_5.1/database/s/s_11.html
Дата изменения: Thu Sep 15 16:56:07 2005 Дата индексирования: Sat Dec 22 13:54:12 2007 Кодировка: Поисковые слова: reflection nebula |
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 (n=2): Edlen, B., 1985, Phys. Scr., 31, 345 %Observed energy levels (22-24,37,39-43,45,46,67,72): Ralchenko Y., Jou, F.C., Kelleher, D.E., Kramida, A.E., Musgrove, A., Reader, J., Wiese, W.L., Olsen, K., 2005, NIST Atomic Spectra Database, Version 3.0 %Observed energy levels (35,36,44): Bromage, G.E., Fawcett, B.C., 1977, MNRAS, 178, 605 %Observed energy levels (28,31,32,64,68): Lepson et al, 2005, ApJ, 625, 1045 %Theoretical energy levels: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - March 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 (n=2): Edlen, B., 1985, Phys. Scr., 31, 345 %Observed energy levels (22-24,37,39-43,45,46,67,72): Ralchenko Y., Jou, F.C., Kelleher, D.E., Kramida, A.E., Musgrove, A., Reader, J., Wiese, W.L., Olsen, K., 2005, NIST Atomic Spectra Database, Version 3.0 %Observed energy levels (35,36,44): Bromage, G.E., Fawcett, B.C., 1977, MNRAS, 178, 605 %Observed energy levels (28,31,32,64,68): Lepson et al, 2005, ApJ, 625, 1045 %Theoretical energy levels: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251 %oscillator strengths and A values: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - March 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: s_11.splups %Oscillator strengths: from the 9-conf model of Landi & Bhatia 2003, ApJ, 149, 251 %Effective collision strengths levels 1-6: Conlon, Keenan & Aggarwal, 1992, Phys. Scripta, 45,309 %Collision strengths levels 7-72: from the 9-conf model of Landi & Bhatia 2003, ApJ, 149, 251 %comment: effective collision strengths are provided in the range 5.45 < log T < 7.05 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % E. Landi - Apr 2003
contains the spline fits to the scaled proton collision strengths.
References:
%filename: s_11.psplups %rates: Ryans R.S.I., Foster-Woods V.J, Keenan F.P., Reid R.H.G., 1999, ADNDT 73, 1-42 %energies: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997 %comment: Fits valid for temperatures 4e5 to 3e7 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 10-Sep-2002