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Article
Discovery of a Magnetic Field in the Rapidly-Rotating O-Type Secondary of the Colliding-Wind Binary HD 47129 (Plaskett’s Star).
Monthly Notices of the Royal Astronomical Society (2013)
  • J. H. Grunhut
  • G. A. Wade
  • M. Leutenegger
  • V. Petit
  • G. Rauw
  • C. Neiner
  • F. Martins
  • D. H. Cohen
  • M. Gagné
  • R. Ignace, East Tennessee State University
  • S. Mathis
  • S. E. de Mink
  • A. F. J. Moffat
  • S. Owocki
  • M. Shultz
  • J. Sundqvist
  • MiMeS Collaboration, MiMeS Collaboration
Abstract

We report the detection of a strong, organized magnetic field in the secondary component of the massive O8III/I+O7.5V/III double-lined spectroscopic binary system HD 47129 (Plaskett's star) in the context of the Magnetism in Massive Stars survey. Eight independent Stokes V observations were acquired using the Echelle SpectroPolarimetric Device for the Observations of Stars (ESPaDOnS) spectropolarimeter at the Canada–France–Hawaii Telescope and the Narval spectropolarimeter at the Télescope Bernard Lyot. Using least-squares deconvolution we obtain definite detections of signal in Stokes V in three observations. No significant signal is detected in the diagnostic null (N) spectra. The Zeeman signatures are broad and track the radial velocity of the secondary component; we therefore conclude that the rapidly rotating secondary component is the magnetized star. Correcting the polarized spectra for the line and continuum of the (sharp-lined) primary, we measured the longitudinal magnetic field from each observation. The longitudinal field of the secondary is variable and exhibits extreme values of −810 ± 150 and +680 ± 190 G, implying a minimum surface dipole polar strength of 2850 ± 500 G. In contrast, we derive an upper limit (3σ) to the primary's surface magnetic field of 230 G. The combination of a strong magnetic field and rapid rotation leads us to conclude that the secondary hosts a centrifugal magnetosphere fed through a magnetically confined wind. We revisit the properties of the optical line profiles and X-ray emission – previously interpreted as a consequence of colliding stellar winds – in this context. We conclude that HD 47129 represents a heretofore unique stellar system – a close, massive binary with a rapidly rotating, magnetized component – that will be a rich target for further study.

Publication Date
January 11, 2013
Publisher Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. doi: 10.1093/mnras/sts153
Citation Information
J. H. Grunhut, G. A. Wade, M. Leutenegger, V. Petit, et al.. "Discovery of a Magnetic Field in the Rapidly-Rotating O-Type Secondary of the Colliding-Wind Binary HD 47129 (Plaskett’s Star)." Monthly Notices of the Royal Astronomical Society Vol. 428 Iss. 2 (2013)
Available at: http://works.bepress.com/richard_ignace/73/