Shock Waves and Line-Profile Variation in roAp Stars

Details Shock Waves and Line-Profile Variation in roAp Stars Shock Waves and Line-Profile Variation in roAp Stars

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008pasj...60...63s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.60, No.1, pp.63--76

Other

10

Line: Profiles, Stars: Chemically Peculiar, Stars: Individual (Γ, Equulei), Stars: Oscillations, Stars: Variables: Other

Scientific paper

Line-profile variation of NdIII and PrIII spectrum lines of roAp stars obtained with high spectral resolution and high time resolution seem to be similar to those seen in rapidly rotating B-type line-profile variables: features in the lines appear to move smoothly from blue to red, but return to the blue discontinuously. It has been argued in the past that such behaviour is in disagreement with the oblique-pulsator interpretion of the photometric observations. We point out why that argument is invalid. We propose that the properties of the observed line-profile variation can in principle be explained as a manifestation of a shocked wave train propagating upwards through an acoustically thick layer high in the atmosphere, and demonstrate that it is consistent with the underlying pulsation being an axisymmetric low-degree, probably dipole oscillation more-or-less aligned with the magnetic axis, in accord with the oblique-pulsator model.

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