Formation of Resonant Atomic Lines during Thermonuclear Flashes on Neutron Stars

Abstract

Motivated by the measurement of redshifted Fe H$α$ 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$α$, Ly$α$ and P$α$ lines. From the observed equivalent width of the Fe H$α$ 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$α$ EW $\approx$ 15-20 eV (redshifted 11-15 eV) and the P$α$ EW $\approx$ 4-7 eV (redshifted 3-5 eV) when the H$α$ EW is 10 eV (redshifted 8 eV). The Ly$α$ 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.