Towards understanding rapid line-profile and light variations of early-type stars. II - Confrontation of several possible models with new spectroscopic data on 45 Epsilon Persei

Details Towards understanding rapid line-profile and light variations of early-type stars. II - Confrontation of several possible models with new spectroscopic data on 45 Epsilon Persei Towards understanding rapid line-profile and light variations of early-type stars. II - Confrontation of several possible models with new spectroscopic data on 45 Epsilon Persei

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990baicz..41..273h&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 41, no. 5, Sept. 1990, p. 273-311.

Astronomy and Astrophysics

Astronomy

14

Astronomical Spectroscopy, Binary Stars, Early Stars, High Dispersion Spectrographs, Stellar Envelopes, Stellar Models, Corotation, H Alpha Line, Helium, Kepler Laws, Signal To Noise Ratios

Scientific paper

Several new series of high-dispersion high S/N spectroscopic (He I 6678 and H-alpha) observations of 45 Per obtained in 1988 are analyzed in detail, and the results are compared with the predictions of several working models. The model of surface spots seems very improbable and also the method of sectorial nonradial pulsations meets certain difficulties when applied to the data. The model of corotating circumstellar structures located up to several stellar radii above the stellar photosphere does not lead to any apparent contradictions as far as its geometrical predictions are concerned. However, its ability to produce line-profile variations similar to those observed has never been demonstrated. None of the models is definitely excluded or confirmed by the analysis. Rather, the complexity of the problem is revealed and the necessity of very long continuous series of observations needed to distinguish between the competing models is indicated. The only firm conclusion of the study is that the radial velocity of the star varies.

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