Convection dans les coquilles sphériques et circulation des planètes géantes Convection in spherical shells and general circulation of giant planets. Pierre Drossart LESIA. Collaboration. Proponents : André Mangeney Olivier Talagrand (LMD) Pierre Drossart PhD Students :
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Convection dans les coquilles sphériques et circulation des planètes géantesConvection in spherical shells and general circulation of giant planets
PhD Students :
E. Brottier, A. Abouelainine, V. Lesueur
External collaborations : M. Rieutord, M. Faure, J.I. Yano, …
Time scale : 1986-1996
=> internal convection present
Question: is the general circulation and the banded appearance due to solar heating OR internal heating ?
Dimensionless parameter : E = ratio of emitted to solar heating
e : ratio of conductive time to radiative time
(neglecting compressibility effects, except for thermal dilatation)
Fields : u = velocity, P = pressure, T = temperature, = vorticity
Characteristic numbers :
T = Taylor, Coriolis vs viscosity
P = Prandtl , ratio of diffusivities
F = Froude, centrifugal force vs gravity
=> Exact comparison possible with Chandrasekhar calculations
unstable spherical harmonics
Deep circulation can be maintained by solar heating at the boundary condition !
…. a lot of fun