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The stretching of magnetic flux tubes in the convective overshoot regionThe present study examines the fate of a magnetic flux tube initially lying at the bottom of the solar convective overshoot region. Stretching of the flux tube, e.g., by differential rotation, reduces its density, causing it to rise quasi-statically (a process referred to as vertical flux drift) until it reaches the top of the overshoot region and enters the buoyantly unstable convection region, from which a portion of it may ultimately protrude to form an active region on the surface. It is suggested that vertical flux drift and flux destabilization are inevitable consequences of field amplification, and it is surmised that these phenomena should be considered in self-consistent models of solar and stellar dynamos operating in the overshoot region.
Document ID
19910056285
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Fisher, George H.
(Hawaii Univ. Honolulu, HI, United States)
Mcclymont, Alexander N.
(Hawaii, University Honolulu, United States)
Chou, Dean-Yi
(Tsing Hua University Hsinchu, Republic of China, United States)
Date Acquired
August 15, 2013
Publication Date
June 20, 1991
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 374
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
91A40908
Funding Number(s)
CONTRACT_GRANT: NSF ATM-88-22366
CONTRACT_GRANT: NSC-78-0208-M007-110
CONTRACT_GRANT: NAGW-864
CONTRACT_GRANT: AF-AFOSR-90-0116
Distribution Limits
Public
Copyright
Other

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