Diffusion and line asymmetries in HgMn stars

Details Diffusion and line asymmetries in HgMn stars Diffusion and line asymmetries in HgMn stars

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..592m&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 592-599. Research supported by the Conseil National de Recherches du

Astronomy and Astrophysics

Astrophysics

15

A Stars, Atmospheric Diffusion, Line Shape, Stellar Atmospheres, Stellar Spectra, Abundance, Astronomical Spectroscopy, Asymmetry, Stellar Models, Velocity Distribution

Scientific paper

If abundance anomalies are caused by diffusion in stellar atmospheres, some elements are expected to lie in thin layers above the stellar atmospheres. It is shown in this paper that line asymmetries are then expected to appear, even in stable atmospheres, but only in the lines of some elements. The velocity distribution for those elements is nonisotropic and non-Maxwellian. The line asymmetries can mimic a stellar wind but without destabilization of the whole atmosphere. This may explain the recent observations of Smith and Parsons (1975, 1976). This model predicts that He and O lines should not show the asymmetry. More observations are needed to confirm or rule out this model.

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