On the Center Shifts of Raman Scattered He II and H$α$ Wings in Symbiotic Stars
Using a Monte Carlo technique, we investigate the center shifts that are expected to occur for the broad H$α$ wings and the He II $λ$ 6545 feature as a function of the neutral hydrogen column density in symbiotic stars.These two features are proposed to be formed via Raman scattering of UV continuum around Ly$β$ and He II $λ$ 1025 emission line by neutral hydrogen. The branching ratio of Raman scattering to Rayleigh scattering for UV radiation around Ly$β$ is a non-linearly increasing function of the wavelength, which results in enhanced Raman optical fluxes redward of the H$α$ line center as $N_{HI}$ increases. However, we find that the amount of wing center shift is quite small about $20{\rm km s^{-1}}$ as $N_{HI}$ increases from $10^{20}{\rm cm^{-2}}$ to $10^{21}{\rm cm^{-2}}$. Assuming that He II $λ$~1025 emission is characterized by a Gaussian profile, the Raman scattered He II 6545 feature exhibits near Gaussian profiles with the peak shifted redward for $N_{HI}<10^{22}{\rm cm^{-2}}$. The redward center shift amounts to $1{\rm Å}$ for $N_{HI}\sim 10^{20}{\rm cm^{-2}}$ and decreases as $N_{HI}$ increases up to $N_{HI}\sim 10^{22}{\rm cm^{-2}}$, above which no center shift is observed. The redward peak shift is due to the fact that the incident emission profile is symmetric with respect to He II $λ$~1025 line center whereas the Raman conversion rate is increasing towards the line center of Ly$β$. We emphasize that the determination of $N_{HI}$ by locating the exact peak position of the He II 6545 feature will lift the degeneracy to allow a more accurate estimate of the covering factor of the neutral region, providing strong constraints on the mass loss process occurring in symbiotic stars.