O IV - VERSION 11.0

The CHIANTI database has the following primary ASCII files for this ion:

  1. o_4.elvlc (energy levels)

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

     

Observed energies (level 2): Feuchtgruber et al. (1997, ApJ, 487, 962).

Observed energies (levels 3,4,5): from the Skylab UV wavelengths measured by 
 Sandlin et al. (1986, APJSS, 61, 801), with about 5 mA accuracy.
     
Other observed energies: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). 
      NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/

Theoretical energies:
G Y Liang, N R Badnell and G Zhao  A&A 547, A87 (2012)
   DOI: 10.1051/0004-6361/201220277
 
 Produced for the CHIANTI database v.8 by Giulio Del Zanna  Aug 2015

26-Jul-2022, Peter Young
  The experimental energies of 6 levels were mis-assigned in the previous file. The
  following levels have been exchanged:
    27 <-> 29
    28 <-> 30
    51 <-> 52

 -1

  2. o_4.wgfa (radiative data)

    3. 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. 

     

Theoretical energies, gf and A-values:
G Y Liang, N R Badnell and G Zhao  A&A 547, A87 (2012)
   DOI: 10.1051/0004-6361/201220277

Note: only transitions with an A-value  above 10^-5 the maximum have been retained.

Observed energies (level 2): Feuchtgruber et al. (1997, ApJ, 487, 962).

Observed energies (levels 3,4,5): from the Skylab UV wavelengths measured by 
 Sandlin et al. (1986, APJSS, 61, 801), with about 5 mA accuracy.
     
Other observed energies: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). 
      NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/

A-values for transitions from levels 3-20 are from Correge, G. & Hibbert, A. 2004, ADNDT, 86, 19
      
Produced for the CHIANTI database v.8 by Giulio Del Zanna  August 2015

Removed the unphysical 114-129 and 114-131 transitions
(observed energy of the upper level lower than the energy of the lower level)
G. Del Zanna 5 May 2016

 
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on 26-Jul-2022
%File processed with wgfa_tidy by pryoung on 31-May-2023

  3. o_4.scups (electron collision data)

    4. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992). 

     
                                                                
 Produced for the CHIANTI database v.8 by G. Del Zanna Oct  2014

Note: data for levels 8,9 have been corrected.                  

   DOI: 10.1051/0004-6361/201220277                             
G Y Liang, N R Badnell and G Zhao  A&A 547, A87 (2012)          
 Data from

  4. o_4.psplups (proton collision data)

    5. contains the spline fits to the scaled proton collision strengths. 

     

%filename: o_4.psplups
%rates: Foster VJ, Keenan FP, Reid RHG, ADNDT 67, 99, 1997
%energies: From .elvlc file, experimental energies
%comment: The rate coefficients are in units cm^3/s.
%comment: Fits valid for temperatures 2e4 to 3e5 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

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

    Page created by Giulio Del Zanna on Tue Dec 3 13:24:51 2024