3. The previous simulation – run1_gs – used the 15 most cosmically abundant elements, but in equal fractions; atomic models were ground states only for all ion stages; 20000 K plasma temperature, 30000 K radiation and spectral temperatures; ion density 1e10. The next simulation – run2_gs – uses the cosmic abundances at: http://dosxx.colorado.edu/~bagenal/1010/graphics/CosmicAbund.html; but ever other setting is the same. http://dosxx.colorado.edu/~bagenal/1010/graphics/CosmicAbund.html

6. Next, we’ll test the importance of including excited levels. We’ll use different CNO models, with one n=2 level and one n=3 level (or so) for the two most abundant ionization stages for each of the elements: C: +3, +4 N: +3, +4 O: +2, +3 One ion stage atm selection is shown for each element on the following three slides Run/workspace is called run1_few_excited

10. The populations in those excited levels is tiny…

11. Looks very, very similar to the ground-states only model (run2_gs) – except for the lines; maybe should choose b-f in the ‘output’ screen of the workspace.