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τ Sco: the discovery of the clones

Published online by Cambridge University Press:  12 July 2011

Véronique Petit
Affiliation:
Dept. of Geology & Astronomy, West Chester University, West Chester, PA 19383, USA email: VPetit@wcupa.edu
Derck L. Massa
Affiliation:
Space Telescope Science Institute, 3700 N. San Martin Drive, Baltimore, MD 21218, USA
Wagner L. F. Marcolino
Affiliation:
Observatório Nacional-MCT, CEP 20921-400, São Cristóvão, Rio de Janeiro, Brasil
Gregg A. Wade
Affiliation:
Dept. of Physics, Royal Military College of Canada, Kingston, Canada, K7K 4B4
Richard Ignace
Affiliation:
Dept. of Physics & Astronomy, East Tennessee State University, Johnson City, TN 37614, USA
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Abstract

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The B0.2 V magnetic star τ Sco stands out from the larger population of massive magnetic OB stars due to its remarkable, superionized wind, apparently related to its peculiar magnetic field – a field which is far more complex than the mostly-dipolar fields usually observed in magnetic OB stars. τ Sco is therefore a puzzling outlier in the larger picture of stellar magnetism – a star that still defies interpretation in terms of a physically coherent model.

Recently, two early B-type stars were discovered as τ Sco analogues, identified by the striking similarity of their UV spectra to that of τ Sco, which was – until now – unique among OB stars. We present the recent detection of their magnetic fields by the MiMeS collaboration, reinforcing the connection between the presence of a magnetic field and a superionized wind. We will also present ongoing observational efforts undertaken to establish the precise magnetic topology, in order to provide additional constrains for existing models attempting to reproduce the unique wind structure of τ Sco-like stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

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