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dc.contributorDepartment of Physics, Engineering Physics and Astronomy, Queen's University, 64 Bader lane, Kingston, K7L 3N6, ON Canada
dc.contributorDepartment of Physics and Space Science, Royal Military College of Canada, PO Box 17000, Stn Forces, Kingston, K7K 7B4, ON, Canada
dc.contributorGroupe d'Astrophysique des Hautes Énergies, Institut d'Astrophysique et de Géophysique Department AGO, Université de Liège, Allée du 6 Août 19c B5c, 4000 Sart Tilman, Belgium
dc.contributorLMU München, Universitätssternwarte Scheinerstr. 1, D-81679 München, Germany
dc.contributorArmagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, U.K
dc.contributorAstronomical Observatory, University of Warsaw, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland
dc.contributor.authorMunoz, M. S.
dc.contributor.authorWade, G. A.
dc.contributor.authorNazé, Y.
dc.contributor.authorPuls, J.
dc.contributor.authorBagnulo, S.
dc.contributor.authorSzymański, M. K.
dc.date.accessioned2024-02-21T11:03:02Z
dc.date.available2024-02-21T11:03:02Z
dc.date.issued2020-02-01T00:00:00Z
dc.identifier.doi10.1093/mnras/stz2904
dc.identifier.doi10.48550/arXiv.1910.05792
dc.identifier.other2019arXiv191005792M
dc.identifier.other2019MNRAS.tmp.2573M
dc.identifier.otherastro-ph.SR
dc.identifier.otherarXiv:1910.05792
dc.identifier.other10.48550/arXiv.1910.05792
dc.identifier.other2020MNRAS.492.1199M
dc.identifier.other2019MNRAS.tmp.2573M
dc.identifier.other10.1093/mnras/stz2904
dc.identifier.other2019arXiv191005792M
dc.identifier.other0000-0002-2534-7292
dc.identifier.other-
dc.identifier.other0000-0002-7156-8029
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1735
dc.description.abstractIn this paper, we investigate the photometric variability of magnetic O-type stars. Such stars possess oblique, predominantly dipolar magnetic fields that confine their winds roughly axisymmetrically about the magnetic equator, thus forming a magnetosphere. We interpret their photometric variability as phase-dependent magnetospheric occultations. For massive star winds dominated by electron scattering opacity in the optical and NIR, we can compute synthetic light curves from simply knowing the magnetosphere's mass density distribution. We exploit the newly-developed Analytical Dynamical Magnetosphere model (ADM) in order to obtain the predicted circumstellar density structures of magnetic O-type stars. The simplicity in our light curve synthesis model allows us to readily conduct a parameter space study. For validation purposes, we first apply our algorithm to HD 191612, the prototypical Of?p star. Next, we attempt to model the photometric variability of the Of?p-type stars identified in the Magellanic Clouds using OGLE photometry. We evaluate the compatibility of the ADM predictions with the observed photometric variations, and discuss the magnetic field properties that are implied by our modelling.
dc.publisherMonthly Notices of the Royal Astronomical Society
dc.titleModelling the photometric variability of magnetic massive stars with the Analytical Dynamical Magnetosphere model
dc.typearticle
dc.source.journalMNRAS
dc.source.journalMNRAS.492
dc.source.volume492
refterms.dateFOA2024-02-21T11:03:02Z
dc.identifier.bibcode2020MNRAS.492.1199M


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