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Article: A three-dimensional multilayered spherical dynamic interface dynamo using the malkus-proctor formulation

TitleA three-dimensional multilayered spherical dynamic interface dynamo using the malkus-proctor formulation
Authors
KeywordsSun: magnetic fields
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 682 n. 2, p. 1392-1403 How to Cite?
AbstractWe investigate a fully three-dimensional and multilayered spherical dynamic interface dynamo using a finite-element method based on the three-dimensional tetrahedralization of the whole spherical system. The dynamic interface dynamo model consists of four magnetically coupled zones: an electrically conducting and uniformly rotating core, a thin differentially rotating tachocline, a turbulent convection envelope, and a nearly insulating exterior. In the thin tachocline at the base of the convection zone, a differential rotation, similar to that of the observed solar differential rotation, is imposed. In the convection zone, the Malkus-Proctor formulation with a prescribed α-effect is employed while the fully three-dimensional dynamic feedback of Lorentz forces is taken into account. Our numerical simulations of the dynamic interface dynamo are focused on the Taylor number Ta = 105 with a unity magnetic Prandtl number. It is shown that the dynamic interface dynamo, depending on the size of the magnetic Reynolds number Rem based on the differential rotation, can be either nonaxisymmetric or axisymmetric. When Rem is small or moderate, the dynamic dynamo is characterized by quasi-periodic and nonaxisymmetric azimuthally traveling waves. When Re m is sufficiently large, the dynamo is characterized by a strong toroidal magnetic field, axisymmetric or nearly axisymmetric, that selects dipolar symmetry and propagates equatorward. Implications of our dynamic interface dynamo for the solar dynamo are also discussed. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/58978
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorChan, KHen_HK
dc.contributor.authorLiao, Xen_HK
dc.contributor.authorZhang, Ken_HK
dc.date.accessioned2010-05-31T03:40:42Z-
dc.date.available2010-05-31T03:40:42Z-
dc.date.issued2008en_HK
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 682 n. 2, p. 1392-1403en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/58978-
dc.description.abstractWe investigate a fully three-dimensional and multilayered spherical dynamic interface dynamo using a finite-element method based on the three-dimensional tetrahedralization of the whole spherical system. The dynamic interface dynamo model consists of four magnetically coupled zones: an electrically conducting and uniformly rotating core, a thin differentially rotating tachocline, a turbulent convection envelope, and a nearly insulating exterior. In the thin tachocline at the base of the convection zone, a differential rotation, similar to that of the observed solar differential rotation, is imposed. In the convection zone, the Malkus-Proctor formulation with a prescribed α-effect is employed while the fully three-dimensional dynamic feedback of Lorentz forces is taken into account. Our numerical simulations of the dynamic interface dynamo are focused on the Taylor number Ta = 105 with a unity magnetic Prandtl number. It is shown that the dynamic interface dynamo, depending on the size of the magnetic Reynolds number Rem based on the differential rotation, can be either nonaxisymmetric or axisymmetric. When Rem is small or moderate, the dynamic dynamo is characterized by quasi-periodic and nonaxisymmetric azimuthally traveling waves. When Re m is sufficiently large, the dynamo is characterized by a strong toroidal magnetic field, axisymmetric or nearly axisymmetric, that selects dipolar symmetry and propagates equatorward. Implications of our dynamic interface dynamo for the solar dynamo are also discussed. © 2008. The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectSun: magnetic fieldsen_HK
dc.titleA three-dimensional multilayered spherical dynamic interface dynamo using the malkus-proctor formulationen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=682&spage=1392&epage=1403&date=2008&atitle=A+Three-Dimensional+Multilayered+Spherical+Dynamic+Interface+Dynamo+Using+the+Malkus-Proctor+Formulationen_HK
dc.identifier.emailChan, KH:mkhchan@hku.hken_HK
dc.identifier.authorityChan, KH=rp00664en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1086/588748en_HK
dc.identifier.scopuseid_2-s2.0-53549085737en_HK
dc.identifier.hkuros146418en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-53549085737&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume682en_HK
dc.identifier.issue2en_HK
dc.identifier.spage1392en_HK
dc.identifier.epage1403en_HK
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000258026100063-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridChan, KH=7406033542en_HK
dc.identifier.scopusauthoridLiao, X=7202134147en_HK
dc.identifier.scopusauthoridZhang, K=7404451892en_HK

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