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SUMMARY:Magnetohydrodynamic shallow-water turbulence on the sphere - Cho\,
  JYK (QMUL)
DTSTART:20081209T163000Z
DTEND:20081209T170000Z
UID:TALK15620@talks.cam.ac.uk
CONTACT:Mustapha Amrani
DESCRIPTION:Motivated by astrophysical-geophysical applications\, we have 
 performed a series of high Reynolds number simulations of magnetohydrodyna
 mic shallow-water turbulence (MHDSWT) on a rotating sphere. MHDSWT is the 
 simplest turbulence model that allows the effects of differential rotation
 \, stratification and magnetic field to be studied over long simulation ti
 mes. A systematic exploration of the full physical and numerical parameter
 -space shows novel as well as consistent behavior\, compared with those of
  pure hydrodynamic (HD) and 2-D MHD counterparts. In the case without rota
 tion and weak magnetic field strength\, the turbulent evolution is sensiti
 ve to initial conditions\, with the strongest dependence on the peak of th
 e initial energy spectrum. With increasing magnetic field strength\, the f
 low field is more susceptible to loss of balance\, and the field blows up 
 in finite time. In addition\, the pronounced zonal structures observed in 
 differentially-rotating HD systems do not form.
LOCATION:Seminar Room 1\, Newton Institute
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