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The pulsating magnetosphere of the extremely slowly rotating magnetic beta Cep star xi(1) CMa
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational 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 Paris Cite, PSL Res Univ,CNRS,Sorbonne Univ,LESIA,Observ Pari, 5 Pl Jules Janssen, F-92195 Meudon, France..
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2017 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 471, no 2, 2286-2310 p.Article in journal (Refereed) Published
Abstract [en]

xi(1) CMa is a monoperiodically pulsating, magnetic beta Cep star with magnetospheric X-ray emission that, uniquely amongst magnetic stars, is clearly modulated with the star's pulsation period. The rotational period P-rot has yet to be identified, with multiple competing claims in the literature. We present an analysis of a large ESPaDOnS data set with a 9 yr baseline. The longitudinal magnetic field < B-z > shows a significant annual variation, suggesting that Prot is at least of the order of decades. The possibility that the star's Ha emission originates around a classical Be companion star is explored and rejected based upon Very Large Telescope Interferometer AMBER and PIONIER interferometry, indicating that the emission must instead originate in the star's magnetosphere and should therefore also be modulated with Prot. Period analysis of Ha equivalent widths measured from ESPaDOnS and CORALIE spectra indicates P-rot > 30 yr. All evidence thus supports that xi(1) CMa is a very slowly rotating magnetic star hosting a dynamical magnetosphere. Ha also shows evidence for modulation with the pulsation period, a phenomenon that we show cannot be explained by variability of the underlying photospheric line profile, i.e. it may reflect changes in the quantity and distribution of magnetically confined plasma in the circumstellar environment. In comparison to other magnetic stars with similar stellar properties, xi(1) CMa is by far the most slowly rotating magnetic B-type star, is the only slowly rotating B-type star with a magnetosphere detectable in Ha ( and thus, the coolest star with an optically detectable dynamical magnetosphere), and is the only known early-type magnetic star with Ha emission modulated by both pulsation and rotation.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2017. Vol. 471, no 2, 2286-2310 p.
Keyword [en]
stars: early-type, stars: individual: xi(1) CMa, stars: magnetic field, stars: mass-loss, stars: oscillations
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-334752DOI: 10.1093/mnras/stx1632ISI: 000409022700069OAI: oai:DiVA.org:uu-334752DiVA: diva2:1160609
Available from: 2017-11-27 Created: 2017-11-27 Last updated: 2017-11-27Bibliographically approved

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Shultz, Matthew

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