Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976pasau...3...75s&link_type=abstract
(Astronomical Society of Australia, Annual General Meeting, 10th, Sydney, Australia, May 12-14, 1976.) Astronomical Society of A
Astronomy and Astrophysics
Astronomy
4
Cepheid Variables, Line Spectra, Spectral Line Width, Stellar Spectra, Stellar Structure, Variable Stars, Algorithms, Light Curve, Limb Darkening, Oscillations, Periodic Variations, Radial Distribution, Stellar Models
Scientific paper
A general algorithm is applied to calculate the form of line profiles expected from radial and nonradial surface oscillations of Beta Cephei stars. The actual form of the stellar surface at any instant during a pulsation is derived by superposing oscillations on an equilibrium surface represented by a rotationally oblated object of 10 solar masses with a polar radius of 7 solar radii and a polar effective temperature of 23,000 K. Limb darkening, full gravity darkening, and a broadening velocity of 8 km/s are assumed. Total line profiles are formed by summing the effects from each of 2500 surface elements with a weight appropriate to the limb darkening at a particular instant during an oscillation and with a Doppler displacement corresponding to the line-of-sight velocity resulting from pulsational and rotational motions. Results are discussed for calculations of the line profiles produced by the m = -2 and m = -1 nonradial modes. It is shown that the m = -2 mode (whose waves can be envisaged as surface bulges which appear to rotate around the star twice per oscillation period) is apparently consistent with the gross features observed in the Beta Cephei group.
Stamford P. A.
Watson Robert D.
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