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Long-Term Photometric and Spectroscopic Monitoring of Slowly Pulsating B Stars1

Published online by Cambridge University Press:  12 April 2016

C. Aerts ,
P. De Cat ,
J. De Ridder ,
K. Kolenberg ,
C. Waelkens ,
P. Mathias  and
M. Briquet
C. Aerts
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
P. De Cat
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
J. De Ridder
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
K. Kolenberg
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
C. Waelkens
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
P. Mathias
Affiliation:
Observatoire de la Côte d’Azur, UMR 6528, Nice, France
M. Briquet
Affiliation:
Institut d’Astrophysique et Géophysique, Université de Liége, Belgium

Abstract

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We review the current status of our long-term monitoring project on slowly pulsating B stars that we started in the course of 1996 and that was recently completed as far as the first part of our plan is concerned. In total, we have selected 17 southern and 8 northern stars. The idea is to fully exploit our current data in the near future and to select the most interesting targets for further very-long-term follow-up monitoring. A first conclusion is that half of the southern targets turn out to be spectroscopic binaries. Some of these have circular orbits and periods of the same order of magnitude as the intrinsic pulsation period(s) of the primary. The eccentric binaries have periods ranging from 12 to 460 d. For most stars the photometric behaviour is dominated by the same frequency as the intrinsic spectroscopic variability. Multiperiodicity in the expected frequency range is found for almost all stars. Two objects, however, turn out to have only one dominant pulsation mode.

Type
Part 6. Variables Close to the Main Sequence
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 394 - 400
Copyright
Copyright © Astronomical Society of the Pacific 2000

Footnotes

2

Postdoctoral Fellow, Fund for Scientific Research, Flanders

1

The follow-up data for the southern stars were gathered with the Swiss Telescope of the Geneva Observatory and with ESO’s CAT telescope, both at La Silla, Chile; those of the northern stars were obtained with the 1.52-m telescope of the Haute-Provence Observatory in France

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