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dc.contributor.authorJeffers, S. V.
dc.contributor.authorMengel, M.
dc.contributor.authorMoutou, C.
dc.contributor.authorMarsden, S. C.
dc.contributor.authorBarnes, J. R.
dc.contributor.authorJardine, M. M.
dc.contributor.authorPetit, P.
dc.contributor.authorSchmitt, J. H. M. M.
dc.contributor.authorSee, V.
dc.contributor.authorVidotto, A. A.
dc.contributor.authorBCool Collaboration
dc.identifier.citationJeffers , S V , Mengel , M , Moutou , C , Marsden , S C , Barnes , J R , Jardine , M M , Petit , P , Schmitt , J H M M , See , V , Vidotto , A A & BCool Collaboration 2018 , ' The relation between stellar magnetic field geometry and chromospheric activity cycles - II The rapid 120-day magnetic cycle of τ Bootis ' , Monthly Notices of the Royal Astronomical Society , vol. 479 , no. 4 , pp. 5266-5271 .
dc.identifier.otherPURE: 255652828
dc.identifier.otherPURE UUID: 590aeb4d-8c89-4083-9b62-13169c1effbf
dc.identifier.otherScopus: 85051484913
dc.identifier.otherWOS: 000441383700071
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821835
dc.descriptionSJ acknowledges support from the German Science Foundation (DFG) Research Unit FOR2544 ‘Blue Planets around Red Stars’, project JE 701/3-1. VS acknowledges funding fromt the European Research Council (ERC) under the European Unions Horizon 2020 research and innovtion programme (grant agreement No 682393 AWESoMeStars).en
dc.description.abstractOne of the aims of the BCool programme is to search for cycles in other stars and to understand how similar they are to the Sun. In this paper, we aim to monitor the evolution of τ Boo's large-scalemagnetic field using high-cadence observations covering its chromospheric activity maximum. For the first time, we detect a polarity switch that is in phase with τ Boo's 120-day chromospheric activity maximum and its inferred X-ray activity cycle maximum. This means that τ Boo has a very fast magnetic cycle of only 240 days. At activity maximum τ Boo's large-scale field geometry is very similar to the Sun at activity maximum: it is complex and there is a weak dipolar component. In contrast, we also see the emergence of a strong toroidal component which has not been observed on the Sun, and a potentially overlapping butterfly pattern where the next cycle begins before the previous one has finished.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectStars: activityen
dc.subjectStars: individual: (τ Boo)en
dc.subjectStars: magnetic fielden
dc.subjectStars: solar-typeen
dc.subjectTechniques: polarimetricen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.titleThe relation between stellar magnetic field geometry and chromospheric activity cycles - II The rapid 120-day magnetic cycle of τ Bootisen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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