Rayleigh Scattering in atmospheres of the Hot-Stars
Jakub Fišák (PřF MU Brno)
The Rayleigh scattering is mostly neglected in the hot star atmosphere
models.
The Rayleigh scattering originates from the interaction of light with atoms
having bound electrons. All hydrogen atoms are almost ionized and heavier
elements have low abundance relatively to hydrogen. In the atmospheres of
some
chemically peculiar stars the helium overabundant regions are present and
Rayleigh scattering could be a significant opacity source. In this work we
show
the contribution of the Rayleigh scattering on neutral hydrogen and singly
ionized helium in the atmospheres of stars with solar composition and for
helium
overabundant stars (N(He)/N(H)=10). We conclude that the Rayleigh scattering
should be included in the model atmospheres of B stars, especially in the
case
of helium strong stars.
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