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dc.contributor.authorWade, Gregg A.
dc.contributor.authorShultz, Matthew E.
dc.contributor.authorSikora, J.
dc.contributor.authorBernier, M.E.
dc.contributor.authorRivinius, Th H.
dc.contributor.authorAlécian, Evelyne
dc.contributor.authorPetit, Véronique
dc.contributor.authorGrunhut, Jason H.
dc.contributor.authorThe BinaMIcS Collaboration
dc.date.accessioned2017-10-18T17:07:48Z
dc.date.available2017-10-18T17:07:48Z
dc.date.issued2016-10-21
dc.identifier.citationWade, G.A., Shultz, M., Sikora, J., Bernier, M.-E., Rivinius, T., Alecian, E., Petit, V., Grunhut, J.H., the BinaMIcS collaboration HD 164492C: A rapidly rotating, Hα-bright, magnetic early B star associated with a 12.5 d spectroscopic binary (2017) Monthly Notices of the Royal Astronomical Society, 465 (3), pp. 2517-2530. Cited 1 time.en_US
dc.identifier.urihttp://hdl.handle.net/11141/2089
dc.descriptionStars: magnetic field, Stars: massive, Stars: rotationen_US
dc.description.abstractWe employ high-resolution spectroscopy and spectropolarimetry to derive the physical properties and magnetic characteristics of the multiple systemHD164492C, located in the young open cluster M20. The spectrum reveals evidence of three components: a broad-lined early B star (HD 164492C1), a narrow-lined early B star (HD 164492C2) and a late B star (HD 164492C3). Components C2 and C3 exhibit significant (>100 km s-1) bulk radial velocity variations with a period of 12.5351(7) d that we attribute to eccentric binary motion around a common centreof- mass. Component C1 exhibits no detectable radial velocity variations. Using constraints derived from modelling the orbit of the C2+C3 binary and from synthesis of the combined spectrum, we determine the approximate physical characteristics of the components. We conclude that a coherent evolutionary solution consistent with the published age of M20 implies a distance to M20 of 0.9 ± 0.2 kpc, corresponding to the smallest published values. We confirm the detection of a strong magnetic field in the combined spectrum. The field is clearly associated with the broad-lined C1 component of the system. Repeated measurement of the longitudinal magnetic field allows the derivation of the rotation period of the magnetic star, Prot =1.369 86(6) d.We derive the star's magnetic geometry, finding i = 63 ± 6°, β = 33 ± 6° and a dipole polar strength Bd = 7.9-1.0 +1.2 kG. Strong emission - varying according to the magnetic period - is detected in the Hα profile. This is consistent with the presence of a centrifugal magnetosphere surrounding the rapidly rotating magnetic C1 component. © 2016 The Authors.en_US
dc.language.isoen_USen_US
dc.rights© 2016 the Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_US
dc.rights.urihttps://academic.oup.com/journals/pages/access_purchase/rights_and_permissions/self_archiving_policy_pen_US
dc.titleHD 164492C: A rapidly rotating, Hα-bright, magnetic early B star associated with a 12.5 d spectroscopic binaryen_US
dc.typeArticleen_US
dc.identifier.doi10.1093/mnras/stw2799


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