Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasp..103.1250k&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 103, Dec. 1991, p. 1250-1257. Research supported by NSE
Astronomy and Astrophysics
Astronomy
18
Cepheid Variables, Stellar Models, Stellar Oscillations, Stellar Rotation, Line Spectra, Radial Velocity, Starspots, Stellar Spectra, Stellar Spectrophotometry, Ubv Spectra
Scientific paper
A sectorial nonradial pulsation model is used to construct theoretical line profiles which mimic the variations for Kappa(2) Boo. Synthetic spectra generated with the appropriate Teff and log g are used as input. It is found that the data can be reproduced by the combination of a high-degree l is approximately equal to 12 mode with P(osc) aproximately equal to 0.071 d, and a low-degree mode, l is approximately equal to 0-2 with P(osc) approximately equal to 0.071-0.079 d. The projected rotational velocity (v sin i - 115 +/-5 km/s) was determined by fitting synthetic line profiles to the observed spectra. The velocity amplitude of the high-degree oscillations is estimated to be about 3.5 km/s. It is found that the ratio of the horizontal and radial pulsation amplitudes is small (about 0.02) and consistent with p-mode oscillations. Comparisons are made with models invoking starspots, and it is impossible to fit the observations of Kappa(2) Boo by a starspot model without assuming unrealistic values of radius or equatorial velocity.
Hubeny Ivan
Kennelly Edward J.
Walker Gordon A. H.
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