  Motivated by the measurement of redshifted Fe H$\alpha$ lines during type I
X-ray bursts on EXO 0748-676 (Cottam, Paerels & Mendez), we study the formation
of atomic Fe lines above the photosphere of a bursting neutron star ($k_BT_{\rm
eff} \approx 1-2 {\rm keV}$). We discuss the effects of Stark broadening,
resonant scattering and NLTE (level population) on the formation of hydrogenic
Fe H$\alpha$, Ly$\alpha$ and P$\alpha$ lines. From the observed equivalent
width of the Fe H$\alpha$ line, we find an implied Fe column of $1-3 \times
10^{20} {\rm cm}^{-2}$, which is 3-10 times larger than the Fe column
calculated from the accretion/spallation model of Bildsten, Chang & Paerels. We
also estimate that the implied Fe column is about a factor of 2-3 larger than a
uniform solar metallicity atmosphere. We discuss the effects of rotational
broadening and find that the rotation rate of \EXO must be slow, as confirmed
by the recent measurement of a 45 Hz burst oscillation by Villarreal &
Strohmayer. We also show that the Fe Ly$\alpha$ EW $\approx$ 15-20 eV
(redshifted 11-15 eV) and the P$\alpha$ EW $\approx$ 4-7 eV (redshifted 3-5 eV)
when the H$\alpha$ EW is 10 eV (redshifted 8 eV). The Ly$\alpha$ line is
rotationally broadened to a depth of $\approx 10%$, making it difficult to
observe with {\it Chandra}. We also show that radiative levitation can likely
support the Fe column needed to explain the line.
