Excitation of the oscillations in roAp stars: Magnetic fields, diffusion, and winds

Details Excitation of the oscillations in roAp stars: Magnetic fields, diffusion, and winds Excitation of the oscillations in roAp stars: Magnetic fields, diffusion, and winds

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..224..359c&link_type=abstract

The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004. Edited by J. Zverko, J. Ziznovsky, S.J. Adelman, and W.W. Weiss,

Physics

1

Stars: Chemically Peculiar, Stars: Magnetic Fields, Stars: Oscillations.

Scientific paper

We discuss different physical aspects that may influence pulsation stability in rapidly oscillating Ap stars. We pay particular attention to the role of the magnetic field, atomic diffusion and winds and point out some of the important uncertainties involved in present studies of pulsation stability in these stars. We argue that presently the models that best reproduce the observations are those with convection suppressed, diffusion of helium, and no winds. With these models, in the region of the HR diagram where most roAp stars have been found, we predict the excitation of high order modes and the damping of low order modes, in accord with observations.

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