The mechanism of the light variability of chemically peculiar stars
2009
Until recently, the mechanism of the light variability of
chemically peculiar (CP) stars was unclear. To improve this
situation, we started a theoretical and observational campaign
aimed at the nature of the light variability of these stars. We
use the TLUSTY model atmospheres calculated for the appropriate
surface chemical composition to obtain the emergent flux and to
predict the rotationally modulated light curves. We show on
example of several well-studied CP stars that their light
variations can be explained as a result of i) the uneven
surface distribution of the elements (creating overabundant
regions), ii) the flux redistribution from the ultraviolet to
the visible part of the spectrum (in the overabundant regions),
and iii) rotation of the star. We show that the silicon and
helium bound-free transitions and iron bound-bound transitions
provide the main contribution to the flux redistribution. This
result is also a very precise test of modern stellar model
atmospheres. We conclude that the mentioned mechanism is a very
promising explanation for the light variations in CP stars of
earlier spectral types.
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