CERN Program Library Long Writeup W5013 - CERNLIB ...

The Auger or Coster-Kronig transitions are represented by the most probable line for a given vacancy [31].
The emitted electron energy E e is
E e = E i − (E j + E k ) (11)
where E i ,E j ,E k are the subshell binding energies and E j >E k .
In case of fluorescence we use transition rates of Scofield [32]. We use only those transitions for which the
occurrence probability is not less than 1%. The fluorescent photon is emitted with energy E γ
E γ = E i − E j (12)
for transition between the subshells i and j.
In addition to the above, to fulfill the energy conservation law, emission of an additional photon is simulated.
For non-radiative transitions its energy is E k (see formula 11). In case of fluorescent transition this photon
has energy E j (see equation 12). The angular distribution of the emitted particle is isotropic.
PHYS231 – 4 227