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The constant magnetic field of ξ1 CMa: geometry or slow rotation?

Published online by Cambridge University Press:  12 July 2011

Chloé Fourtune-Ravard ,
Gregg A. Wade ,
Wagner L. F. Marcolino ,
Matthew Shultz ,
Jason H. Grunhut  and
Huib F. Henrichs
Chloé Fourtune-Ravard
Affiliation:
Université Paris Diderot-Paris 7, UFR de Physique, France email: c.fourtune.ravard@gmail.com Department of Physics, Royal Military College of Canada, Ontario, Canada
Gregg A. Wade
Affiliation:
Department of Physics, Royal Military College of Canada, Ontario, Canada
Wagner L. F. Marcolino
Affiliation:
LAM-UMR 6110, CNRS & Univ. de Provence, France Observatòrio Nacional, Rio de Janeiro, Brazil
Matthew Shultz
Affiliation:
Department of Physics, Engineering Physics & Astronomy, Queen's University, Canada
Jason H. Grunhut
Affiliation:
Department of Physics, Royal Military College of Canada, Ontario, Canada Department of Physics, Engineering Physics & Astronomy, Queen's University, Canada
Huib F. Henrichs
Affiliation:
Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands
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Abstract

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We report recent observations of the sharp-lined magnetic βCep pulsator ξ1 CMa (= HD 46328). The longitudinal magnetic field of this star is detected consistently, but it is not observed to vary significantly, during nearly 5 years of observation. In this poster we evaluate whether the constant longitudinal field is due to intrinsically slow rotation, or rather if the stellar or magnetic geometry is responsible.

Keywords

stars: magnetic fieldsstars: rotationstars: early-typestars: individual (ξ1 CMa)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 180 - 181
Copyright
Copyright © International Astronomical Union 2011

References

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