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HD66051: the first eclipsing binary hosting an early-type magnetic star
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium.
Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France.
Royal Mil Coll Canada, Dept Phys & Space Sci, POB 17000, Kingston, ON K7K 7B4, Canada.
2018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 478, no 2, p. 1749-1762Article in journal (Refereed) Published
Abstract [en]

Early-type magnetic stars are rarely found in close binary systems. No such objects were known in eclipsing binaries prior to this study. Here we investigated the eclipsing, spectro-scopic double-lined binary HD66051, which exhibits out-of-eclipse photometric variations suggestive of surface brightness inhomogeneities typical of early-type magnetic stars. Using a new set of high-resolution spectropolarimetric observations, we discovered a weak magnetic field on the primary and found intrinsic, element-dependent variability in its spectral lines. The magnetic field structure of the primary is dominated by a nearly axisymmetric dipolar component with a polar field strength B-d approximate to 600G and an inclination with respect to the rotation axis of beta(d) = 13 degrees. A weaker quadrupolar component is also likely to be present. We combined the radial velocity measurements derived from our spectra with archival optical photometry to determine fundamental masses (3.16 and 1.75 M-circle dot) and radii (2.78 and 1.39 R-circle dot) with a 1-3 per cent precision. We also obtained a refined estimate of the effective temperatures (13000 and 9000 K) and studied chemical abundances for both components with the help of disentangled spectra. We demonstrate that the primary component of HD66051 is a typical late-B magnetic chemically peculiar star with a non-uniform surface chemical abundance distribution. It is not an HgMn-type star as suggested by recent studies. The secondary is a metallic-line star showing neither a strong, global magnetic field nor intrinsic spectral variability. Fundamental parameters provided by our work for this interesting system open unique possibilities for probing interior structure, studying atomic diffusion, and constraining binary star evolution.

Place, publisher, year, edition, pages
Oxford University Press, 2018. Vol. 478, no 2, p. 1749-1762
Keywords [en]
binaries: eclipsing, stars: chemically peculiar, stars: fundamental parameters, stars: individual: HD66051 (V414 Pup), stars: magnetic field
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-362046DOI: 10.1093/mnras/sty1118ISI: 000439547400022OAI: oai:DiVA.org:uu-362046DiVA, id: diva2:1255318
Funder
Knut and Alice Wallenberg FoundationSwedish Research CouncilEU, European Research Council, 670519: MAMSIEAvailable from: 2018-10-11 Created: 2018-10-11 Last updated: 2018-12-11

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Kochukhov, Oleg

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