The identification of 3d-4p and 3d-4f transitions in Fe IX-XIV in the solar spectrum

It is suggested that previously unidentified lines in the solar spectrum between 170 Angstrom and 70 Angstrom are due to transitions of the type 3p n -1 3d-3p n -1 4p and 3p n -1 3d-3p n -1 4f in Fe IX-XIV, and that the lines are formed by spontaneous radiative decay following collisional transitions from 3p n to 3p n -1 4p and 3p n -1 4f. The contribution of cascades from the 4p and 4f levels to the population of the 4s and 3d levels is estimated to be approximately 12% and 4% respectively.