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Applications of Non-Adiabatic Radial Pulsation Equations to roAp Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
We apply a code that solves grey radial non-adiabatic pulsation equations with consistent treatment of radiative transfer to the roAp frequency regime. We find evidence for the existence of chromospheric modes at frequencies 2.5 mHz, 3.7 mHz, 4.6 mHz and 5.7 mHz in the equilibrium model we used. We also find that, since the oscillations are not adiabatic at the surfaces of roAp stars, better surface boundary conditions need to be considered in future studies.
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- Part 2.3. Chemically Peculiar Stars
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- Copyright © Astronomical Society of the Pacific 2002
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