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A numerical study of dynamo action as a function of spherical shell geometry
 

Summary: A numerical study of dynamo action as a function
of spherical shell geometry
M.H. Heimpela,*, J.M. Aurnoub
, F.M. Al-Shamalia,1
, N. Gomez Pereza
a
Department of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2J1
b
Department of Earth and Space Sciences, University of California, Los Angeles, 90095-1567, USA
Received 20 September 2004; received in revised form 24 February 2005; accepted 8 April 2005
Available online 17 June 2005
Editor: S. King
Abstract
The geometry of the liquid region of a planetary core can effect core convection and magnetic field generation processes.
Varying the spherical shell radius ratio, v =ri /ro, illustrates differences between planets with differing core radius ratios as well
as how dynamo processes vary with time in an evolving planetary core. Here we study numerical models of thermally driven
dynamo action in a rotating shell of outer radius ro with electrically conducting Boussinesq fluid that surrounds an equally
conductive solid inner sphere of radius ri. Dynamo solutions are found for 0.15Vv V0.65 at Ekman number E =3104
,
Prandtl number Pr =1, and magnetic Prandtl number Pm =5, with mechanically rigid, isothermal boundary conditions. In cases

  

Source: Aurnou, Jonathan - Department of Earth and Space Sciences, University of California at Los Angeles

 

Collections: Geosciences