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Atomic diffusion has been recognized as an important process that has to beconsidered in any computations of stellar models. In solar-type and coolerstars, this process is dominated by gravitational settling, which is nowincluded in most stellar evolution codes. In hotter stars, radiativeaccelerations compete with gravity and become the dominant ingredient in thediffusion flux for most heavy elements. Introducing radiative accelerationsinto the computations of stellar models modifies the internal elementdistribution and may have major consequences on the stellar structure. Couplingthese processes with hydrodynamical stellar motions has important consequencesthat need to be investigated in detail. We aim to include the computations ofradiative accelerations in a stellar evolution code (here the TGEC code) usinga simplified method (SVP) so that it may be coupled with sophisticatedmacroscopic motions. We also compare the results with those of the Montrealcode in specific cases for validation and study the consequences of thesecoupled processes on accurate models of A- and early-type stars. We implementedradiative accelerations computations into the Toulouse-Geneva stellar evolutioncode following the semi-analytical prescription proposed by Alecian andLeBlanc. This allows more rapid computations than the full description used inthe Montreal code. We present results for A-type stellar models computed withthis updated version of TGEC and compare them with similar published modelsobtained with the Montreal evolution code. We discuss the consequences for thecoupling with macroscopic motions, including thermohaline convection.

The new Toulouse-Geneva Stellar Evolution Code including radiative accelerations of heavy elements