BEGIN:VCALENDAR
VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-1049
DTSTART:20080229T220000Z
DURATION:PT1H0M0S
DTSTAMP:20260423T055204Z
LAST-MODIFIED:19700101T060000Z
LOCATION:2241 Chamberlin Hall (coffee at 3:30 pm)
SUMMARY:Probing the sources of solar magnetism with helioseismology an
 d simulations\, Physics Department Colloquium\, Juri Toomre\, JILA and
  Dept Astrophysical & Planetary Sciences\, University of Colorado
DESCRIPTION:There exist major challenges to understand how the Sun bui
 lds the large-scale and intense magnetic fields that we observe at its
  surface and how these fields evolve in time. The origin of these magn
 etic fields must rest with dynamo processes occurring deep within the 
 star. Many complex dynamical elements are involved in the operation of
  the solar global dynamo.  These include the differential rotation of 
 the convection zone and the tachocline at its base\, turbulent product
 ion and transport of the magnetic fields by the convection\, shear amp
 lification of the fields\, and magnetic buoyancy that leads to the eve
 ntual field eruption onto the photosphere.  Major advances in supercom
 puting are allowing us to improve the fidelity with which we can model
  these intensely turbulent processes. These efforts are aided by conti
 nuing guidance provided by helioseismology in probing dynamics in the 
 solar interior. We discuss the close interplay between helioseismology
  and recent 3-D simulations in studying the solar global dynamo.
URL:https://www.physics.wisc.edu/events/?id=1049
END:VEVENT
END:VCALENDAR