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The magnetic early B-type stars I: magnetometry and rotation
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy. Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.;Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.;ESO European Org Astron Res Southern Hemisphere, Casilla 19001, Santiago 19, Chile..
Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada..
ESO European Org Astron Res Southern Hemisphere, Casilla 19001, Santiago 19, Chile..
Univ Paris Diderot, UPMC Univ Paris 06, Sorbonne Univ,Observ Paris, PSL Res Univ,CNRS,LESIA,Sorbonne Paris Cite, 5 Pl Jules Janssen, F-92195 Meudon, France..
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2018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 475, no 4, p. 5144-5178Article in journal (Refereed) Published
Abstract [en]

The rotational and magnetic properties of many magnetic hot stars are poorly characterized, therefore the Magnetism in Massive Stars and Binarity and Magnetic Interactions in various classes of Stars collaborations have collected extensive high-dispersion spectropo-larimetric data sets of these targets. We present longitudinal magnetic field measurements < B-z > for 52 early B-type stars (B5-B0), with which we attempt to determine their rotational periods P-rot. Supplemented with high-resolution spectroscopy, low-resolution Dominion As-trophysical Observatory circular spectropolarimetry, and archival Hipparcos photometry, we determined P-rot for 10 stars, leaving only five stars for which P-rot could not be determined. Rotational ephemerides for 14 stars were refined via comparison of new to historical magnetic measurements. The distribution of P-rot is very similar to that observed for the cooler Ap/Bp stars. We also measured v sin i and v(mac) for all stars. Comparison to non-magnetic stars shows that v sin i is much lower for magnetic stars, an expected consequence of magnetic braking. We also find evidence that v(mac) is lower for magnetic stars. Least-squares deconvolution profiles extracted using single-element masks revealed widespread, systematic discrepancies in < B-z > between different elements: this effect is apparent only for chemically peculiar stars, suggesting it is a consequence of chemical spots. Sinusoidal fits to H line < B-z > measurements (which should be minimally affected by chemical spots), yielded evidence of surface magnetic fields more complex than simple dipoles in six stars for which this has not previously been reported; however, in all six cases, the second- and third-order amplitudes are small relative to the first-order (dipolar) amplitudes.

Place, publisher, year, edition, pages
Oxford University Press, 2018. Vol. 475, no 4, p. 5144-5178
Keywords [en]
magnetic fields, stars: chemically peculiar, stars: early-type, stars: magnetic field, stars: massive, stars: rotation
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-351693DOI: 10.1093/mnras/sty103ISI: 000428835700060OAI: oai:DiVA.org:uu-351693DiVA, id: diva2:1213089
Available from: 2018-06-04 Created: 2018-06-04 Last updated: 2018-06-04Bibliographically approved

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Shultz, Matthew E.

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