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The periods of the β Cephei star κ Scorpii as observed by WIRE

Published online by Cambridge University Press:  12 April 2016

J. Cuypers ,
D. Buzasi  and
K. Uytterhoeven
J. Cuypers
Affiliation:
Koninklijke Sterrenwacht van België, Ringlaan 3, B-1180, Brussels, Belgium
D. Buzasi
Affiliation:
Department of Physics, US Air Force Academy, Colorado Springs, CO 80840, USA
K. Uytterhoeven
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium

Abstract

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The β Cephei star κ Scorpii is known to be multiperiodic from old photometric observations. A main period of 4.8 hr was detected, and from a beat period of about 7 d a secondary period of 4.9 hr was calculated. These periods were also found in recently analyzed line profile data. In two short data sets (separated by 152 d) obtained by the star camera of the satellite WIRE (Wide-field Infrared Explorer) the known main period of 4.8 hr is clearly present. The secondary period could also be confirmed, although some other periodicities are present as well. While the amplitude of the main variation is about 0.0055 mag, the amplitude of the secondary is only 0.0014 mag. Two longer periods (3.6 and 0.45 d) and a period of 4.2 hr were also found significant in the WIRE data.

Type
Part 4. Early-type stars: B, A and F pulsators
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 251 - 254
Copyright
Copyright © Astronomical Society of the Pacific 2004

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