Radiative levitation of silicon in the atmospheres of two Hyades DA white dwarfs

Abstract

Abstract The presence of silicon at the surface of the two Hyades DA white dwarfs WD 0421+162 and WD 0431+126 requires mechanisms that counteract the effects of the downward diffusion. Radiative levitation calculations indicate that the silicon abundance observed in WD 0431+126 corresponds to the abundance supported by radiative levitation. Detailed time-dependent diffusion calculations that take into account radiative levitation and accretion indicate that accretion with rates of $\dot{M}_{\rm {Si}} \lesssim 10^4$ g s−1 could also be present without disrupting the abundance supported by radiative levitation. In the case of WD 0421+162, accretion with a rate of $\dot{M}_{\rm {Si}} = 10^{5.1}$ g s−1 must be invoked, because its observed silicon abundance is larger than the abundance supported by radiative levitation. This accretion rate is lower than the accretion rate given by the accretion–diffusion model, because the radiative levitation slows down the downward diffusion of silicon. The silicon abundances observed in the two Hyades white dwarfs cannot be interpreted solely in terms of accretion. The interpretation of the silicon abundances must take into account the interplay between radiative levitation and accretion.