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MOBSTER - III. HD62658: a magnetic Bp star in an eclipsing binary with a non-magnetic 'identical twin'
Univ Delaware, Dept Phys & Astron, 217 Sharp Lab, Newark, DE 19716 USA.
Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium.
Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, BR-05508900 Sao Paulo, SP, Brazil.
Univ Delaware, Dept Phys & Astron, 217 Sharp Lab, Newark, DE 19716 USA.
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 490, no 3, p. 4154-4165Article in journal (Refereed) Published
Abstract [en]

HD62658 (B9p V) is a little-studied chemically peculiar star. Light curves obtained by the Kilodegree Extremely Little Telescope (KELT) and Transiting Exoplanet Survey Satellite (TESS) show clear eclipses with a period of about 4.75 d, as well as out-of-eclipse brightness modulation with the same 4.75 d period, consistent with synchronized rotational modulation of surface chemical spots. High-resolution ESPaDOnS circular spectropolarimetry shows a clear Zeeman signature in the line profile of the primary; there is no indication of a magnetic field in the secondary. PHOEBE modelling of the light curve and radial velocities indicates that the two components have almost identical masses of about 3 M-circle dot. The primary's longitudinal magnetic field < B-z > varies between about +100 and -250 G, suggesting a surface magnetic dipole strength B-d = 850 G. Bayesian analysis of the Stokes V profiles indicates B-d = 650 G for the primary and B-d < 110 G for the secondary. The primary's line profiles are highly variable, consistent with the hypothesis that the out-of-eclipse brightness modulation is a consequence of rotational modulation of that star's chemical spots. We also detect a residual signal in the light curve after removal of the orbital and rotational modulations, which might be pulsational in origin; this could be consistent with the weak line profile variability of the secondary. This system represents an excellent opportunity to examine the consequences of magnetic fields for stellar structure via comparison of two stars that are essentially identical with the exception that one is magnetic. The existence of such a system furthermore suggests that purely environmental explanations for the origin of fossil magnetic fields are incomplete.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2019. Vol. 490, no 3, p. 4154-4165
Keywords [en]
binaries: eclipsing, stars: chemically peculiar, stars: early-type, stars: individual: HD 62658, stars: magnetic field
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-402659DOI: 10.1093/mnras/stz2846ISI: 000503993100076OAI: oai:DiVA.org:uu-402659DiVA, id: diva2:1386994
Funder
EU, Horizon 2020, 670519: MAMSIEKnut and Alice Wallenberg FoundationSwedish Research Council, 621-2014-5720Swedish National Space Board, 185/14Swedish National Space Board, 137/17Available from: 2020-01-20 Created: 2020-01-20 Last updated: 2020-01-20Bibliographically approved

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Kochukhov, Oleg

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