EDP Sciences
Free Access
Volume 475, Number 3, December I 2007
Page(s) 1053 - 1065
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20078189

A&A 475, 1053-1065 (2007)
DOI: 10.1051/0004-6361:20078189

Weak magnetic fields in Ap/Bp stars

Evidence for a dipole field lower limit and a tentative interpretation of the magnetic dichotomy
M. Aurière1, G. A. Wade2, J. Silvester2, 3, F. Lignières1, S. Bagnulo4, K. Bale2, B. Dintrans1, J. F. Donati1, C. P. Folsom2, M. Gruberbauer5, A. Hui Bon Hoa1, S. Jeffers6, N. Johnson2, J. D. Landstreet7, A. Lèbre8, T. Lueftinger5, S. Marsden9, D. Mouillet1, S. Naseri1, F. Paletou1, P. Petit1, J. Power2, F. Rincon1, S. Strasser10, and N. Toqué11

1  Laboratoire d'Astrophysique de Toulouse-Tarbes, Université Paul Sabatier, CNRS, Observatoire Midi-Pyrénées, 57 avenue d'Azereix, 65008 Tarbes, France
    e-mail: michel.auriere@ast.obs-mip.fr
2  Department of Physics, Royal Military College of Canada, PO Box 17000, Station "Forces", Kingston, Ontario, Canada K7K 4B4
3  Department of Physics, Queen's University, Kingston, Ontario, Canada
4  Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland
5  Institut für Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Wien, Austria
6  Sterrekundig Instituut Utrecht, Universiteit Utrecht, PO Box 80000, 3508 TA Utrecht, The Netherlands
7  Department of Physics & Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7
8  GRAAL, Université Montpellier II, CNRS, 62 place Eugène Bataillon, 34095 Montpellier, France
9  Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia
10  Department of Astronomy, University of Minnesota, 116 Church Street, S.E., Minneapolis 55455, USA
11  Department of Physics and Astronomy, Saint Mary's University, 923 Robie Street, Halifax, Nova Scotia, B3H3C3, Canada

(Received 29 June 2007 / Accepted 17 September 2007 )

Aims.We investigated a sample of 28 well-known spectroscopically-identified magnetic Ap/Bp stars, with weak, poorly-determined or previously undetected magnetic fields. The aim of this study is to explore the weak part of the magnetic field distribution of Ap/Bp stars.
Methods.Using the MuSiCoS and NARVAL spectropolarimeters at Télescope Bernard Lyot (Observatoire du Pic du Midi, France) and the cross-correlation technique Least Squares Deconvolution (LSD), we obtained 282 LSD Stokes V signatures of our 28 sample stars, in order to detect the magnetic field and to infer its longitudinal component with high precision (median $\sigma=40$ G).
Results.For the 28 studied stars, we obtained 27 detections of Stokes V Zeeman signatures from the MuSiCoS observations. Detection of the Stokes V signature of the $28{\rm th}$ star (HD 32650) was obtained during science demonstration time of the new NARVAL spectropolarimeter at Pic du Midi. This result clearly shows that when observed with sufficient precision, all firmly classified Ap/Bp stars show detectable surface magnetic fields. Furthermore, all detected magnetic fields correspond to longitudinal fields which are significantly greater than some tens of G. To better characterise the surface magnetic field intensities and geometries of the sample, we phased the longitudinal field measurements of each star using new and previously-published rotational periods, and modeled them to infer the dipolar field intensity ($B_{\rm d}$, measured at the magnetic pole) and the magnetic obliquity ($\beta$). The distribution of derived dipole strengths for these stars exhibits a plateau at about 1 kG, falling off to larger and smaller field strengths. Remarkably, in this sample of stars selected for their presumably weak magnetic fields, we find only 2 stars for which the derived dipole strength is weaker than 300 G. We interpret this "magnetic threshold" as a critical value necessary for the stability of large-scale magnetic fields, and develop a simple quantitative model that is able to approximately reproduce the observed threshold characteristics. This scenario leads to a natural explanation of the small fraction of intermediate-mass magnetic stars. It may also explain the near-absence of magnetic fields in more massive B and O-type stars.

Key words: stars: chemically peculiar -- stars: magnetic fields

© ESO 2007

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