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Investigating the Magnetospheres of Rapidly Rotating B-type Stars
Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32904 USA.
Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA.
Univ Liege, FNRS GAPHE, STAR, Inst Astrophys & Geophys B5C, Allee 6 Aout 19c, B-4000 Liege, Belgium.
Royal Mil Coll Canada, Dept Phys, POB 17000 Stn Forces, Kingston, ON K7K 0C6, Canada.
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2017 (English)In: Lives And Death-Throes Of Massive Stars / [ed] Eldridge, JJ; Bray, JC; McClelland, LAS; Xiao, L, 2017, no S329, p. 369-372Conference paper, Published paper (Refereed)
Abstract [en]

Recent spectropolarimetric surveys of bright, hot stars have found that similar to 10% of OB-type stars contain strong (mostly dipolar) surface magnetic fields (similar to kG). The prominent paradigm describing the interaction between the stellar winds and the surface magnetic field is the magnetically confined wind shock (MCWS) model. In this model, the stellar wind plasma is forced to move along the closed field loops of the magnetic field, colliding at the magnetic equator, and creating a shock. As the shocked material cools radiatively it will emit X-rays. Therefore, X-ray spectroscopy is a key tool in detecting and characterizing the hot wind material confined by the magnetic fields of these stars. Some B-type stars are found to have very short rotational periods. The effects of the rapid rotation on the X-ray production within the magnetosphere have yet to be explored in detail. The added centrifugal force due to rapid rotation is predicted to cause faster wind outflows along the field lines, leading to higher shock temperatures and harder X-rays. However, this is not observed in all rapidly rotating magnetic B-type stars. In order to address this from a theoretical point of view, we use the X-ray Analytical Dynamical Magnetosphere (XADM) model, originally developed for slow rotators, with an implementation of new rapid rotational physics. Using X-ray spectroscopy from ESA's XMM-Newton space telescope, we observed 5 rapidly rotating B-types stars to add to the previous list of observations. Comparing the observed X-ray luminosity and hardness ratio to that predicted by the XADM allows us to determine the role the added centrifugal force plays in the magnetospheric X-ray emission of these stars.

Place, publisher, year, edition, pages
2017. no S329, p. 369-372
Series
IAU Symposium Proceedings Series, ISSN 1743-9213, E-ISSN 1743-9221 ; 12
Keywords [en]
massive stars, magnetic fields, stars, rotation, x-rays
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-377141DOI: 10.1017/S1743921317002812ISI: 000455603400061ISBN: 978-1-10717-006-3 (print)OAI: oai:DiVA.org:uu-377141DiVA, id: diva2:1289439
Conference
329th Symposium of the International-Astronomical-Union (IAU), NOV 28-DEC 02, 2016, Auckland, NEW ZEALAND
Available from: 2019-02-18 Created: 2019-02-18 Last updated: 2019-02-18Bibliographically approved

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Shultz, Matthew

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