Iron Convection Zones in B, A, and F Stars

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Abstract
Stellar models, including all effects of atomic diffusion and radiative accelerations, are evolved from the pre-main sequence to the giant branch for stars of 1.3 to 4.0 M☉, with metallicity ranging from Z0 = 0.01 to 0.03. It is shown that radiative accelerations lead to the accumulation of iron-peak elements around 200,000 K; this increases the opacity and causes the appearance of Fe convection zones when macroscopic motions are not rapid enough to wipe out the effects of particle transport. The behavior of Fe convection zones and conditions for their appearance are studied in detail. Iron-peak convection zones appear naturally in all solar metallicity models more massive than 1.5 M☉. In the 1.5 M☉ model, it is present only for a fraction of the main-sequence lifetime, but in models without turbulence of 1.7 M☉ and more, the Fe convection zone rapidly develops after arrival on the main-sequence and remains until its end. For a metallicity of Z = 0.01, an Fe convection zone appears even in a 1.3 M☉ model. Moreover, the interaction between the diffusion velocities of different species leads to an accumulation of heavy elements around the convective core, causing semiconvection. A detached semiconvection zone develops in the 1.5 M☉ model. Finally, the surface abundances are calculated using a number of turbulence models and compared to observations of τ UMa in order to show how abundance anomalies may be used to test various turbulence models; the gravity at which abundance anomalies should be expected to disappear is determined. It is shown that in Am stars, the Ca underabundance should disappear during evolution at the same gravity as iron-peak overabundances.