Element stratification in the atmospheres of main sequence stars - The silicon accumulation

Details Element stratification in the atmospheres of main sequence stars - The silicon accumulation Element stratification in the atmospheres of main sequence stars - The silicon accumulation

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...101...16a&link_type=abstract

Astronomy and Astrophysics, vol. 101, no. 1, Aug. 1981, p. 16-25.

Astronomy and Astrophysics

Astrophysics

59

Atmospheric Stratification, Magnetic Stars, Main Sequence Stars, Silicon, Stellar Atmospheres, Stellar Magnetic Fields, Stellar Structure, Abundance, Atmospheric Diffusion, Autoionization, Stellar Models, Stellar Temperature

Scientific paper

Calculations are presented of silicon diffusion in the atmospheres of chemically peculiar main sequence stars in the presence and absence of a magnetic field. The radiative accelerations of silicon atoms and ions in stellar atmospheres are computed for stellar models with effective temperatures of 12,000 and 14,000 K as a function of depth in the atmosphere and horizontal magnetic field strength, and it is found that only in the presence of a magnetic field is the acceleration great enough in the line formation region to produce large Si overabundances. The abundance anomalies to be expected in the case of magnetic lines parallel to the stellar surface are then examined and calculated in detail for the case of an effective temperature of 12,000 K and a horizontal field of 10,000 G, and the effects of diffusion across oblique magnetic lines are considered. On the basis of the present results, a model is proposed for magnetic Ap stars in which elements in the neutral state suspended by the magnetic field accumulate around regions of horizontal field lines in the atmosphere, while ionized elements accumulate at regions of horizontal field lines further above the stellar surface.

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