dc.contributor.author |
Gokhale, M. H |
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dc.contributor.author |
Hiremath, K. M |
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dc.date.accessioned |
2008-07-21T09:06:41Z |
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dc.date.available |
2008-07-21T09:06:41Z |
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dc.date.issued |
1993-04-10 |
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dc.identifier.citation |
Astrophysical Journal, Vol. 407, No. 1, Part 1, pp. 359 - 366 |
en |
dc.identifier.issn |
0004-637X |
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dc.identifier.uri |
http://hdl.handle.net/2248/2755 |
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dc.description.abstract |
We model the structure of the 'steady' (slowest varying) part of the sun's internal poloidal magnetic field assuming it to be (for given reasons and in the relevant domain) a current-free field whose field lines 'isorotate' according to the sun's internal rotation given by helioseismology. This part of the field can be described as that of a central dipole and a central hexapole both parallel to the rotation axis and embedded in a uniform external field. The field structure contains a critical surface (running along the base of the convection zone in the low latitudes), where a discontinuity of about 7 nHz per unit flux in the gradient of rotation may be winding a poloidal field into a toroidal field about 2 MG in about 10 exp 5 - 10 exp 9 yr. Small deviations from isorotation indicate presence of MHD perturbations whose latitude structure and time scales may be similar to those dominant in the solar cycle. |
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dc.format.extent |
1396937 bytes |
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dc.format.mimetype |
application/pdf |
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dc.language.iso |
en |
en |
dc.publisher |
American Astronomical Society |
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dc.relation.uri |
http://adsabs.harvard.edu/abs/1993ApJ...407..359G |
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dc.subject |
Solar interior |
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dc.subject |
Solar magnetic field |
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dc.subject |
Solar physics |
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dc.subject |
Solar rotation |
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dc.subject |
Helioseismology |
en |
dc.subject |
Stellar models |
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dc.title |
A model of the 'steady' and 'fluctuating' parts of the sun's internal magnetic field |
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dc.type |
Article |
en |