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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:1
UID:UW-Physics-Event-4999
DTSTART:20190311T170500Z
DURATION:PT1H0M0S
DTSTAMP:20260311T075944Z
LAST-MODIFIED:20190301T141121Z
LOCATION:2241 Chamberlin Hall
SUMMARY:Numerical modeling of magnetic self-organization at the top of
  the solar convection zone\, Plasma Physics (Physics/ECE/NE 922) Semin
 ar\, John O'Bryan\, University of Washington-Seattle
DESCRIPTION:Nonlinear\, numerical computation with the NIMROD code is 
 used to explore magnetic self-organization near the narrow\, convectiv
 ely unstable super-adiabatic layer at the top of the solar convection 
 zone.   The convective turbulence produced by the super-adiabatic rapi
 dly saturates with kinetic and magnetic energy fluctuations in equipar
 tition.  Magnetic self-organization produces a radially-localized\, la
 titudinally-elongated magnetic structure.  The convective turbulence d
 rive is stabilized by magnetic field\, which limits the achievable mag
 netic field from localized turbulence alone.  Differential rotation of
  the sun creates an inductive electric field which also causes growth 
 of the magnetic field within the structure\, the rate of which scales 
 with its magnitude.  The saturated small-scale turbulence can also dri
 ve a large-scale dynamo through the magnetic shear-current effect.  Wh
 en considered together\, the localized convective turbulence and rotat
 ional flow shear create a robust mechanism for magnetic field generati
 on\, regardless of its magnitude.  The nonlinear evolution of such a s
 hallow magnetic structure may provide insight into the evolution of su
 rface magnetic features.
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URL:https://www.physics.wisc.edu/events/?id=4999
END:VEVENT
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