We have investigated the origin of the Fe II emission fines in Be star
s using a four level Fe+ model. We have computed the equivalent widths
W-eq of emission due to (I) Fe++ recombination in the H II region sur
rounding the Be star, and (2) photoexcitation and decay of Fe+ in the
C II region, which is outside the H II region. We find that the observ
ed Fe II line emission should arise from the C II region while recombi
nation in the H II region is negligible