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Non-linear and chaotic dynamo regimes
KTH, Centra, Nordic Institute for Theoretical Physics NORDITA.ORCID-id: 0000-0002-7304-021X
2012 (engelsk)Inngår i: Proceedings of the International Astronomical Union: Vol. 8 Symposium S294, Cambridge University Press, 2012, nr S294, 387-398 s.Konferansepaper, Publicerat paper (Fagfellevurdert)
Abstract [en]

An update is given on the current status of solar and stellar dynamos. At present, it is still unclear why stellar cycle frequencies increase with rotation frequency in such a way that their ratio increases with stellar activity. The small-scale dynamo is expected to operate in spite of a small value of the magnetic Prandtl number in stars. Whether or not the global magnetic activity in stars is a shallow or deeply rooted phenomenon is another open question. Progress in demonstrating the presence and importance of magnetic helicity fluxes in dynamos is briefly reviewed, and finally the role of nonlocality is emphasized in modeling stellar dynamos using the mean-field approach. On the other hand, direct numerical simulations have now come to the point where the models show solar-like equatorward migration that can be compared with observations and that need to be understood theoretically.

sted, utgiver, år, opplag, sider
Cambridge University Press, 2012. nr S294, 387-398 s.
Serie
Proceedings of the International Astronomical Union, ISSN 1743-9213 ; 8
Emneord [en]
MHD, Sun: magnetic fields, turbulence
HSV kategori
Identifikatorer
URN: urn:nbn:se:kth:diva-125176DOI: 10.1017/S1743921313002822Scopus ID: 2-s2.0-84880530805ISBN: 978-110703383-2 (tryckt)OAI: oai:DiVA.org:kth-125176DiVA: diva2:639499
Konferanse
the International Astronomical Union 2012
Merknad

QC 20130808

Tilgjengelig fra: 2013-08-08 Laget: 2013-08-07 Sist oppdatert: 2013-10-01bibliografisk kontrollert

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