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dc.contributor.authorIşık, Emre
dc.contributor.authorSchmitt, D.
dc.contributor.authorSchuessler, M.
dc.date.accessioned2016-09-06T13:29:02Z
dc.date.available2016-09-06T13:29:02Z
dc.date.issued2011-04
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/11413/1432
dc.description.abstractContext. The Sun and other cool stars harbouring outer convection zones manifest magnetic activity in their atmospheres. The connection between this activity and the properties of a deep-seated dynamo generating the magnetic flux is not well understood. Aims. By employing physical models, we study the spatial and temporal characteristics of the observable surface field for various stellar parameters. Methods. We combine models for magnetic flux generation, buoyancy instability, and transport, which encompass the entire convection zone. The model components are: (i) a thin-layer alpha Omega dynamo at the base of the convection zone; (ii) buoyancy instabilities and the rise of flux tubes through the convection zone in 3D, which provides a physically consistent determination of emergence latitudes and tilt angles; and (iii) horizontal flux transport at the surface. Results. For solar-type stars and rotation periods longer than about 10 days, the latitudinal dynamo waves generated by the deep-seated alpha Omega dynamo are faithfully reflected by the surface distribution of magnetic flux. For rotation periods of the order of two days, however, Coriolis acceleration of rising flux loops leads to surface flux emergence at much higher latitudes than the dynamo waves at the bottom of the convection zone reach. A similar result is found for a K0V star with a rotation period of two days. In the case of a rapidly rotating K1 subgiant, overlapping dynamo waves lead to noisy activity cycles and mixed-polarity fields at high latitudes. Conclusions. The combined model reproduces the basic observed features of the solar cycle. The differences between the latitude distributions of the magnetic field at the bottom of the convection zone and the emerging surface flux grow with increasing rotation rate and convection zone depth, becoming quite substantial for rapidly rotating dwarfs and subgiants. The dynamical evolution of buoyantly rising magnetic flux should be considered as an essential ingredient in stellar dynamo models.tr_TR
dc.language.isoen_UStr_TR
dc.publisherEdp Sciences S A, 17, Ave Du Hoggar, Pa Courtaboeuf, Bp 112, F-91944 Les Ulis Cedex A, Francetr_TR
dc.relationAstronomy & Astrophysicstr_TR
dc.subjectSun: activitytr_TR
dc.subjectSun: dynamotr_TR
dc.subjectstars: interiorstr_TR
dc.subjectstars: late-typetr_TR
dc.subjectstars: activitytr_TR
dc.subjectstars: magnetic fieldtr_TR
dc.subjectsolar convection zonetr_TR
dc.subjectdifferential rotationtr_TR
dc.subjectactivity cyclestr_TR
dc.subjectmain-sequencetr_TR
dc.subjectpolar spotstr_TR
dc.subjecttubestr_TR
dc.subjectdynamotr_TR
dc.subjectsurfacetr_TR
dc.subjectGüneş: etkinliktr_TR
dc.subjectGüneş: dinamotr_TR
dc.subjectyıldız: içtr_TR
dc.subjectyıldız: Geç tiptr_TR
dc.subjectyıldız: etkinliktr_TR
dc.subjectyıldız: manyetik alantr_TR
dc.subjectgüneş konveksiyon bölgesitr_TR
dc.subjectdiferansiyel rotasyontr_TR
dc.subjectetkinlik çevrimleritr_TR
dc.subjectanakoltr_TR
dc.subjectkutup noktalartr_TR
dc.subjecttüplertr_TR
dc.subjectdinamotr_TR
dc.subjectyüzeytr_TR
dc.titleMagnetic Flux Generation And Transport In Cool Starstr_TR
dc.typeArticletr_TR


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