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HD 156324: a tidally locked magnetic triple spectroscopic binary with a disrupted magnetosphere
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
ESO European Org Astron Res Southern Hemisphere, Casilla 19001, Santiago 19, Chile.
Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France;CNRS, IPAG, F-38000 Grenoble, France;Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris,UMR 8109, 5 Pl Jules Janssen, F-92190 Meudon, France.
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2018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 475, no 1, p. 839-852Article in journal (Refereed) Published
Abstract [en]

HD 156324 is an SB3 (B2VIB5VIB5V) system in the Sco OB4 association. The He-strong primary possesses both a strong magnetic field and Ha emission believed to originate in its centrifugal magnetosphere. We analyse a large spectroscopic and high-resolution spectropolarimetric data set. The radial velocities (RVs) indicate that the system is composed of two subsystems, which we designate A and B. Period analysis of the RVs of the three components yields orbital periods P-orb = 1.5806(1) d for the Aa and Ab components, and P-orb = 6.67(2) d for the B component, a PGa star. Period analysis of the longitudinal magnetic field (B,) and H alpha equivalent widths, which should both be sensitive to the rotational period Prot of the magnetic Aa component, both yield 1.58 d. Since P-orb = P-rot Aa and Ab must be tidally locked. Consistent with this, the orbit is circularized, and the rotational and orbital inclinations are identical within uncertainty, as are the semimajor axis and the Kepler corotation radius. The star's Ha emission morphology differs markedly from both theoretical and observational expectations in that there is only one, rather than two, emission peaks. We propose that this unusual morphology may be a consequence of modification of the gravitocentrifugal potential by the presence of the close stellar companion. We also obtain upper limits on the magnetic dipole strength B-d for the Ab and B components, respectively, finding B-d < 2.6 and <0.7 kG.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2018. Vol. 475, no 1, p. 839-852
Keywords [en]
binaries: close, stars: early-type, stars: individual: HD 156324, stars: magnetic field, stars: massive
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-354518DOI: 10.1093/mnras/stx3238ISI: 000427144200066OAI: oai:DiVA.org:uu-354518DiVA, id: diva2:1233521
Available from: 2018-07-18 Created: 2018-07-18 Last updated: 2018-07-18Bibliographically approved

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Shultz, Matthew

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