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SUMMARY:Magnetic buoyancy instabilities in the solar tachocline - Paul Bus
 hby (Newcastle University)
DTSTART:20180604T130000Z
DTEND:20180604T140000Z
UID:TALK82501@talks.cam.ac.uk
CONTACT:Dr. Yufeng Lin
DESCRIPTION:Sunspots are surface manifestations of a large-scale magnetic 
 field that rises to the solar photosphere\, under the action of magnetic b
 uoyancy\, from deep within the solar interior. It is generally accepted th
 at most of the large-scale magnetic flux that appears at the surface origi
 nates from the tachocline\, which is a region of strong differential rotat
 ion around the base of the solar convection zone. Adopting an idealised mo
 del that mimics a local region of the tachocline\, I will discuss magnetic
  buoyancy instabilities in a shear-generated magnetic layer. Recent result
 s suggest that such an instability can only operate in rather restricted r
 egions of parameter space\, which would have serious implications for the 
 solar tachocline\; I will focus particularly upon the extent to which thes
 e results actually constrain the magnetic buoyancy instability in this sys
 tem. Finally\, I will describe some preliminary calculations that suggest 
 that shear-driven magnetic buoyancy may be playing a crucial role in the l
 arge-scale solar dynamo (for which there is still no universally accepted 
 model
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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