Discovery of a strong magnetic field on the O star HD 191612: new clues to the future of θ1 Orionis C

DOI PDF 被引用文献3件
  • J.-F. Donati
    1LATT, Observatoire Midi-Pyrénées, 14 Av. E. Belin, F-31400 Toulouse, France
  • I. D. Howarth
    2Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT
  • J.-C. Bouret
    3LAM, Observatoire Astronomique de Marseille-Provence, Traverse du Siphon BP 8, F-13376 Marseille Cedex 12, France
  • P. Petit
    1LATT, Observatoire Midi-Pyrénées, 14 Av. E. Belin, F-31400 Toulouse, France
  • C. Catala
    4LESIA, CNRS-UMR 8109, Observatoire de Paris, 5 Place Janssen, F-92195 Meudon Cedex, France
  • J. Landstreet
    5Department of Physics and Astronomy, University of Western Ontario, London, Ontario N6A 3K7, Canada

書誌事項

公開日
2006-01-01
DOI
  • 10.1111/j.1745-3933.2005.00115.x
公開者
Oxford University Press (OUP)

この論文をさがす

説明

<jats:title>Abstract</jats:title> <jats:p>From observations made with the ESPaDOnS spectropolarimeter, recently installed on the 3.6-m Canada-France-Hawaii Telescope, we report the discovery of a strong magnetic field in the Of?p spectrum variable HD 191612 - only the second known magnetic O star (following θ1 Ori C). The stability of the observed Zeeman signature over four nights of observation, together with the non-rotational shape of line profiles, argues that the rotation period of HD 191612 is significantly longer than the 9-d value previously proposed. We suggest that the recently identified 538-d spectral variability period is the rotation period, in which case the observed line-of-sight magnetic field of −220 ± 38 G implies a large-scale field (assumed dipolar) with a polar strength of about −1.5 kG. If confirmed, this scenario suggests that HD 191612 is, essentially, an evolved version of the near-zero-age main-sequence magnetic O star θ1 Ori C, but with an even stronger field (about 15 kG at an age similar to that of θ1 Ori C). We suggest that the rotation rate of HD 191612, which is exceptionally slow by accepted O-star standards, could be due to angular momentum dissipation through a magnetically confined wind.</jats:p>

収録刊行物

被引用文献 (3)*注記

もっと見る

詳細情報 詳細情報について

問題の指摘

ページトップへ