Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210..219k&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 219-221 (IAU Colloquium 134)
Astronomy and Astrophysics
Astrophysics
1
Cepheid Variables, Early Stars, Stellar Oscillations, Stellar Rotation, Astronomical Spectroscopy, Periodic Variations, Stellar Spectra
Scientific paper
The line-profile variations have been found in many early-type stars surrounding the classical beta Cephei variables in the H-R diagram. The feature of the variations has not been known enough mainly because of their periods of about one day. To specify the cause of the variations, however, it is necessary to make clear their features such as the multi-periodicity, the relation between the photometric variations and the spectroscopic ones, and the cause of existence or non-existence of mode (or period) switching (Balona 1991, Smith 1991). In Be stars, the correlation of the amplitude of the variations with their emission cycle is also important (Ando 1986). We have been extensively monitoring the line-profile variations in a Be star, zeta Oph, a prototype of the line-profile variables to investigate their features (Vogt and Penrod 1983, Harmanec 1989). We have already shown that the variations could be reproduce well by two nonradial pulsations (NRPs) throughout oor observations between 1987 and 1990. The correlation of the amplitudes of NRPs with its Be emission cycle is also found in the star. In this paper, we discuss the NRPs in May 1991, about one year after its latest emission episode.
Ando Hiroki
Hirata Ryuko
Kambe Eiji
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