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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-1376
DTSTART:20081216T213000Z
DURATION:PT1H0M0S
DTSTAMP:20260506T200014Z
LAST-MODIFIED:20081212T152718Z
LOCATION:6515 Sterling Hall
SUMMARY:Dynamos and Magnetism in Rapidly Rotating Suns\, Astronomy Col
 loquium\, Ben Brown\, University of Colorado
DESCRIPTION:When stars like our Sun are young\, they rotate much faste
 r than the Sun currently does. These rapidly rotating suns are observe
 d to have strong magnetic fields\, which likely arise from dynamo acti
 on in their turbulent convection zones. We explore stellar dynamos wit
 h 3-D simulations of turbulent convection in rotating spherical shells
  using the anelastic spherical harmonic (ASH) code. These simulated st
 ars build strong magnetic fields in the bulk of their convection zone.
  This is in striking contrast to our understanding of the solar dynamo
 \, where we think a tachocline of shear at the base of the convection 
 zone is a crucial ingredient for the global-scale dynamo.
URL:https://www.physics.wisc.edu/events/?id=1376
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