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The Be star omicron Cassiopeiae

Published online by Cambridge University Press:  12 April 2016

Pavel Koubský ,
Hasan Ak ,
Petr Harmanec ,
Stephenson Yang  and
Hrvoje Božić
Pavel Koubský
Affiliation:
Astronomical Institute, Ondřejov Observatory, 251 65 Ondřejov, Czech Republic
Hasan Ak
Affiliation:
Ankara University Observatory, 06100 Tandoğan, Ankara, Turkey
Petr Harmanec
Affiliation:
Astronomical Institute, Ondřejov Observatory, 251 65 Ondřejov, Czech Republic Astronomical Institute of the Charles University, 180 00 Praha 8, Czech Republic
Stephenson Yang
Affiliation:
University of Victoria, Victoria, B.C. V8W 3P6, Canada
Hrvoje Božić
Affiliation:
Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kačićeva 26, 10000 Zagreb, Croatia

Abstract

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The analysis of radial velocities (RVs) of the Be star ο Cas from 27 high S/N spectra allowed us to revive the binary nature of this star, first suggested by Abt & Levy (1978, “AL”), but later refuted by several authors. The period search in our RV data based on measurements of Hα emission and He I λ6678 Å absorption profiles detected a dominant peak close to the 1033-d period found by AL. The resulting curves are very smooth. The rms error of the solution for the emission RVs is nearly 5 times lower than the scatter of the solution by AL. If the RV variations are due to orbital motion, then ο Cas turns out to be a challenging system with an unseen secondary component with mass comparable to, or even more massive than the primary.

Type
Part 6. Binary stars and pulsation
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 387 - 390
Copyright
Copyright © Astronomical Society of the Pacific 2004

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