Fe XIII - VERSION 4.0

The CHIANTI database consists of 4 primary ASCII files for each ion in the database.

• fe_13.elvlc (energy levels)

  contains the energy levels in cm^(-1) It includes both experimental data and theoretical values of the levels energies.

  References:

  % filename: fe_13.elvlc
  %observed energy levels(1-3): Penn & Kuhn, 1994, ApJ, 434, 807
  %observed energy levels(6,9- 11,13,15,16,22): Jupen et al., MNRAS, 264, 627, 1993
  %observed energy levels(4-5,7-8,12,14,17-21,23-27): NIST Database for Atomic
     Spectroscopy, Version 1.0, NIST Standard Reference Database 61, 1995.
  %Theoretical energy levels: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
  %Theoretical energy for level 6: Fawcett & Mason, 1989, ADNDT, 43, 245
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
  %
  % E. Landi 2000
  

  
  

• fe_13.wgfa (radiative data)

  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(1-3): Penn & Kuhn, 1994, ApJ, 434, 807
  %observed energy levels(6,9- 11,13,15,16,22): Jupen et al., MNRAS, 264, 627, 1993
  %observed energy levels(4-5,7-8,12,14,17-21,23-27): NIST Database for Atomic
     Spectroscopy, Version 1.0, NIST Standard Reference Database 61, 1995.
  %Theoretical energy levels: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
  % A values: computed from 'superstructure' using a 24 configuration model of Fe XIII.
  % comment: the model of Fe XIII included the following configurations:
      3s2 {3p2 3p3d 3d2}
      3s23p {4s 4p 4d 4f}
      3s3p2 {3d 4s 4p 4d 4f}
      3p3 {3d 4s 4p 4d}
      3s3d {4s 4p 4d 4f}
      3p4
      3s {3p3 3d3 3p3d2}
  % comment: level 18 is metastable, and can decay down to levels
      in the 3s3p^3 and 3s^23p3d configurations via electric quadrupole
      and magnetic dipole transitions. However, the strongest
      transitions are down to the ground configuration via two magnetic
      QUADRUPOLE transitions. These transitions are accurately known
      since the line strength hardly changes when extra configurations
      are added to the model.
  
  % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  %   P.R.Young 1999
  

  
  

• fe_13.splups (electron collision data)

  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_13.splups
  %oscillator strengths: SUPERSTRUCTURE calculation (see file fe_13.wgfa for details)
  % effective collision strengths: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
  %comment: effective collision strengths were given in the temperature range 5.7 < Log T < 6.7
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E. Landi - Apr 1999
  

  
  

• fe_13.psplups (electron collision data)

  contains the spline fits to the scaled proton collision strengths.

  References:

  
  %filename: fe_13.psplups
  %rates: Landman D.A., A&A 43, 285, 1975
  %energies: Landman D.A., A&A 43, 285, 1975
  %comment: Landman tabulates rates between the individual magnetic sublevels of 
      the ground configuration levels. For CHIANTI we sum over these 
      sublevels using Eq. 8 of Landman.
  %comment: These fits reproduce the original data to within 2%. The original 
      data cover the temperature range 1e-6 to 3e-6.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % P.R.Young - Jun 2001
  

The html tables below contain the radiative data of all the lines sorted in wavelength