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Search for the magnetic field of the O7.5 III star ξ Persei

Published online by Cambridge University Press:  01 November 2008

Huib F. Henrichs
Affiliation:
Astronomical Institute, University of Amsterdam, Amsterdam, Netherlands
R. S. Schnerr
Affiliation:
Inst. for Solar Physics, Royal Swedish Academy of Sciences, Stockholm, Sweden
J. A. de Jong
Affiliation:
Max Planck Institute for Extraterrestrial Physics, Garching, Germany
L. Kaper
Affiliation:
Astronomical Institute, University of Amsterdam, Amsterdam, Netherlands
J.-F. Donati
Affiliation:
Observatoire Midi-Pyrénées, Toulouse, France
C. Catala
Affiliation:
LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, Meudon, France
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Abstract

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Cyclical wind variability is an ubiquitous but as yet unexplained feature among OB stars. The O7.5 III(n)((f)) star ξ Persei is the brightest representative of this class on the Northern hemisphere. As its prominent cyclical wind properties vary on a rotational time scale (2 or 4 days) the star has been already for a long time a serious magnetic candidate. As the cause of this enigmatic behavior non-radial pulsations and/or a surface magnetic field are suggested. We present a preliminary report on our attempts to detect a magnetic field in this star with high-resolution measurements obtained with the spectropolarimeter Narval at TBL, France during 2 observing runs of 5 nights in 2006 and 5 nights in 2007. Only upper limits could be obtained, even with the longest possible exposure times. If the star hosts a magnetic field, its surface strength should be less than about 300 G. This would still be enough to disturb the stellar wind significantly. From our new data it seems that the amplitude of the known non-radial pulsations has changed within less than a year, which needs further investigation.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

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