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ξ1 CMa: An Extremely Slowly Rotating Magnetic B0.7 IV Star

Published online by Cambridge University Press:  23 January 2015

Matt Shultz ,
Gregg Wade ,
Thomas Rivinius ,
Wagner Marcolino ,
Huib Henrichs ,
Jason Grunhut  and
the MiMeS Collaboration
Matt Shultz
Affiliation:
European Southern Observatory email: mshultz@eso.org Queen's University, Canada Royal Military College, Canada
Gregg Wade
Affiliation:
Royal Military College, Canada
Thomas Rivinius
Affiliation:
European Southern Observatory email: mshultz@eso.org
Wagner Marcolino
Affiliation:
Observatório do Valongo, UFRJ, Brazil
Huib Henrichs
Affiliation:
Anton Pannekoek Institute for Astronomy, University of Amsterdam, the Netherlands
Jason Grunhut
Affiliation:
European Southern Observatory email: mshultz@eso.org
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Abstract

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We present our analysis of 6 years of ESPaDOnS spectropolarimetry of the magnetic β Cep star ξ1 CMa (B1 III). This high-precision magnetometry is consistent with a rotational period Prot > 40 yr. Absorption line profiles can be reproduced with a non-rotating model. We constrain R⋆, L⋆, and the stellar age via a Baade-Wesselink analysis. Spindown due to angular momentum loss via the magnetosphere predicts an extremely long rotational period if the magnetic dipole Bd > 6 kG, a strength also inferred by the best-fit sinusoids to the longitudinal magnetic field measurements BZ when phased with a 60-year Prot.

Keywords

stars: circumstellar matterstars: magnetic fieldsstars: rotation

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