@article{PAR00008692,
  title = {{A} dynamo driven by zonal jets at the upper surface : applications to giant planets},
  author = {{G}uervilly, {C}. and {C}ardin, {P}hilippe and {S}chaeffer, {N}.},
  editor = {},
  language = {{ENG}},
  abstract = {{W}e present a dynamo mechanism arising from the presence of barotropically unstable zonal jet currents in a rotating spherical shell. {T}he shear instability of the zonal flow develops in the form of a global {R}ossby mode, whose azimuthal wavenumber depends on the width of the zonal jets. {W}e obtain self-sustained magnetic fields at magnetic {R}eynolds numbers greater than 10(3). {W}e show that the propagation of the {R}ossby waves is crucial for dynamo action. {T}he amplitude of the axisymmetric poloidal magnetic field depends on the wavenumber of the {R}ossby mode, and hence on the width of the zonal jets. {W}e discuss the plausibility of this dynamo mechanism for generating the magnetic field of the giant planets. {O}ur results suggest a possible link between the topology of the magnetic field and the profile of the zonal winds observed at the surface of the giant planets. {F}or narrow {J}upiter-like jets, the poloidal magnetic field is dominated by an axial dipole whereas for wide {N}eptune-like jets, the axisymmetric poloidal field is weak.},
  keywords = {{M}agnetic fields ; {J}upiter, {I}nterior ; {N}eptune, {I}nterior ; {R}otational dynamics},
  booktitle = {},
  journal = {{I}carus},
  volume = {218},
  numero = {1},
  pages = {100--114},
  ISSN = {0019-1035},
  year = {2012},
  DOI = {10.1016/j.icarus.2011.11.014},
  URL = {https://www.documentation.ird.fr/hor/{PAR}00008692},
}