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Plaskett’s Star: a fundamental revision of the architecture of the system

Published online by Cambridge University Press:  29 August 2024

E. Stacey Open the ORCID record for E. Stacey [Opens in a new window] ,
G. A. Wade ,
J. H. Grunhut ,
C. P. Folsom  and
O. Kochukhov
E. Stacey*
Affiliation:
Royal Military College of Canada, Kingston, Canada
G. A. Wade
Affiliation:
Royal Military College of Canada, Kingston, Canada
J. H. Grunhut
Affiliation:
Telus Digital, Toronto, Canada
C. P. Folsom
Affiliation:
Tartu Observatory, University of Tartu, Tartu, Estonia
O. Kochukhov
Affiliation:
Uppsala University, Uppsala, Sweden
*
email: erik@erikstacey.com
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Abstract

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A century of study has characterized Plaskett’s Star (HD 47129) as an evolved, massive, short-period, equal mass O+O binary system. The discovery of a magnetic field in the broad-line component by Grunhut et al. (2013) renewed interest in the study of this system and led to its establishment as the most rapidly rotating magnetic O-type star. Grunhut et al. (2021) observed the circular polarization signatures of the magnetic star to exhibit no radial velocity variations while the narrow-line star demonstrates radial velocity variations consistent with the established orbital period. This has raised fundamental questions about the architecture of this system and the nature of the magnetic star which have led to a major shift in our understanding of HD 47129.

Keywords

magnetic starsmassive starsbinary evolution
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 336 - 338
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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