2011A&A...534A..18M

Abundance anomalies observed in a fraction of A and B stars of both Pop I and II are apparently related to internal particle transport. Using available constraints from SiriusA, we wish to determine how well evolutionary models including atomic diffusion can explain observed abundance anomalies when either turbulence or mass loss is used as the main competitor to atomic diffusion. Complete stellar evolution models, including the effects of atomic diffusion and radiative accelerations, have been computed from the zero age main-sequence of 2.1M_☉ stars for metallicities of Z₀=0.01±0.001, and shown to closely reproduce the observed parameters of SiriusA. Surface abundances were predicted for three values of the mass loss rate and four values of the mixed surface zone. A mixed mass of ∼10^–6M_☉ or a mass loss rate of 10^–13M_☉/yr were determined through comparison with observations. There are 17 abundances that were determined observationally and that are included in our calculations. Up to 15 of them can be predicted to within 2σ; three of the four determined upper limits are compatible. While the abundance anomalies can be reproduced slightly better using turbulence as the process competing with atomic diffusion, mass loss probably ought to be preferred since the mass loss rate required to fit abundance anomalies is compatible with the observationally determined rate. A mass loss rate within a factor of 2 of 10^–13M_☉/yr is preferred. This restricts the range of the directly observed mass loss rate.