kaastra and mewe (1993) paper calculates everything that one would ever want to know about what happens after elements with atomic numbers 4 through 30 are ionized this paper was cited by Drain's ISM book which makes it seem like a pretty good source to me the paper is kaastra-mewe.pdf

following ionization, auger electrons as well as fluorescent photons from line transitions are emitted we are interested in the information about fluorescence which is in table 3 table 3 is in table3.txt table 3's columns are --Z: atomic # --ST: initial ionization (1 = neutral...) --S: shell of e- ejected (1 = K... ) --Delta: num auger e- ejected (so total Delta + 1 e- ejected) --IL: fluorescence transition (e.g. Kalpha1, Kalpha2, ...) --E: energy of transition (after all e- ejected) --OMEGA: avg # of photons per ionization (for fixed Z, st, s; all omega sum to less than 1 since sometimes only auger e- produced)

we are interested specifically in the Kalpha line for a handful of elements (C, O, N, Ne, Mg, Si, Fe) L -> K has two possibilities --2s -> 1s (forbidden because delta ell = 0) --2p1/2 -> 1s (this is Kalpha1; in 2p, 2p1/2 is lower energy due to spin-orbit coupling) --2p3/2 -> 1s (this is Kalpha2) in the code, i combine the data for Kalpha1 and Kalpha2 into one data point so that omega = omega_1 + omega_2 and E = (E_1omega_1 + E_2omega_2)/(omega_1 + omega_2) this is because the lines are very close to each other; differing by at most 0.5% for high ionization states of iron

the code is dothing.py it loads and processes table3's data to what we're interested in and makes some plots