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The Nature of Balmer Line Variability in Chemically Peculiar Stars

Published online by Cambridge University Press:  12 April 2016

B. Musielok
B. Musielok*
Affiliation:
Astronomical Institute of the Wroclaw UniveristyKopernika 11 51-622 Wroclaw, Poland

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Photoelectric measurements of the β-index were made for six Ap-stars (56 Ari, 41 Tau, φ Dra, HD 188041, HD 215441, HD 221568) and one He-rich star (HD 184927). For all these stars the minimum of β occurs at a phase of maximum light at a wavelength longward of the null-wavelength region. Such coincidence can be explained by the blanketing mechanism proposed by Kodaira (1973) for the explanation of the Hγ line variations in HD 221568. According to Kurucz (1979), for stars hotter than 9000K an increase of metal abundance in the atmosphere causes an increase of the visible flux and an simultanous decrease of equivalent widths of Balmer lines. The same changes of the visible flux and equivalent widths of Balmer lines can be obtained using a model atmosphere with a suitable higher temperature. Using the Kurucz (1979) model atmospheres, temperature differences were calculated, which are necessary to obtain the observed decrease of the (β-index and the increase of the flux in a given photometric band.

Type
Section II - Systematics, Photometry
Information
International Astronomical Union Colloquium , Volume 90: Upper Main Sequence Stars with Anomalous Abundances , 1986 , pp. 179 - 180
Copyright
Copyright © Reidel 1986

References

Bond, H.E., and Levato, H. 1977. Publ.Astron.Soc.Pacific, 88, 905.Google Scholar
Gulliver, A.F., and Winzer, J.E. 1973, Astrophys.J., 183, 701.Google Scholar
Hardorp, J. 1975, Dudley Obs.Rep., 9, 467.Google Scholar
Khokhlova, V.L. 1972, Soviet Astron.J., 48, 939.Google Scholar
Klinglesmith, D.A. 1971, Hydrogen Line Blanketed Model Stellar Atmospheres, NASA, Washington, D.C. Google Scholar
Kodaira, K. 1973, Astron. Astrophys., 25, 93.Google Scholar
Kurucz, R.L. 1979, Astrophys. J. Suppl., 40, 1.CrossRefGoogle Scholar
Levato, H., and Malaroda, S. 1979, Publ.Astron.Soc.Pacific, 91, 789.Google Scholar
Osmer, P.S., and Peterson, D.M. 1974, Astrophys.J., 187, 117.Google Scholar
Riabchikova, T.A. 1972, Izv. Krym. Astrofiz. Obs., 45, 146.Google Scholar
Weiss, W.W., Albrecht, R., and Wieder, R. 1976, Astron. Astrophys., 47, 423.Google Scholar