Bi-dimensional element stratifications computed for magnetic Ap star atmospheres
Résumé
Context. Theoretical modelling of abundance stratifications and surface distributions of chemical elements in Ap stars constitutes a major challenge. The atomic diffusion model provides the most appropriate framework in which to understand these abundance anomalies.
Aims: We present theoretical 2D stratifications of 16 metals in upper main sequence chemically peculiar stars, with and without magnetic fields to provide a reference point for further theoretical and observational studies.
Methods: We used our code CaratStrat to compute a large grid of stratifications (equilibrium solutions in LTE) for plane-parallel Teff = 8500, 10 000, 12 000, and 14 000 K stellar atmospheres. By interpolation, we constructed bi-dimensional cuts through these stellar atmospheres, which are permeated by a dipolar magnetic field of strength 20 kG at the magnetic pole. We also provide vertical (1D) stratifications of metals in non-magnetic stars (HgMn).
Results: We present a large number of 2D and 1D stratifications, mostly as online material. We discuss in detail the case of Fe for the Teff = 8500 K model in the printed version, and compare it with stratifications derived from observed spectra.
Aims: We present theoretical 2D stratifications of 16 metals in upper main sequence chemically peculiar stars, with and without magnetic fields to provide a reference point for further theoretical and observational studies.
Methods: We used our code CaratStrat to compute a large grid of stratifications (equilibrium solutions in LTE) for plane-parallel Teff = 8500, 10 000, 12 000, and 14 000 K stellar atmospheres. By interpolation, we constructed bi-dimensional cuts through these stellar atmospheres, which are permeated by a dipolar magnetic field of strength 20 kG at the magnetic pole. We also provide vertical (1D) stratifications of metals in non-magnetic stars (HgMn).
Results: We present a large number of 2D and 1D stratifications, mostly as online material. We discuss in detail the case of Fe for the Teff = 8500 K model in the printed version, and compare it with stratifications derived from observed spectra.
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