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SUMMARY:Double-Diffusive Magnetic Buoyancy - Dr. Lara Silvers (City Univer
 sity London)
DTSTART:20131203T130000Z
DTEND:20131203T140000Z
UID:TALK48164@talks.cam.ac.uk
CONTACT:Dr. Jaroslav Dudik
DESCRIPTION:Magnetic buoyancy\, believed to occur in the solar  tachocline
 \, is both an important part of large-scale solar dynamo models and the pi
 cture of how sunspots are formed. Given that in the tachocline region the 
 ratio of magnetic diffusivity to thermal diffusivity is small it is import
 ant\, for both the dynamo and sunspot formation pictures\, to understand m
 agnetic buoyancy in this  egime. Furthermore\, the tachocline is a region 
 of strong shear and such investigations must involve structures that becom
 e buoyant in the double-diffusive regime\, which are generated entirely fr
 om a shear flow. \n\nIn this talk\, I will briefly review my initial  3D-c
 alcuations that showed that a double diffusive  buoyancy instability was p
 ossible in the tachocline. \nHowever\, as I will discuss\, it became appar
 ent that a reduced quasi-two dimensional model needed to be considered. I 
 will then present this model together with the findings from the research.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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