Buoyancy-driven perturbations in a rapidly rotating, electrically conducting fluid: part I - flow and magnetic field

Details Buoyancy-driven perturbations in a rapidly rotating, electrically conducting fluid: part I - flow and magnetic field Buoyancy-driven perturbations in a rapidly rotating, electrically conducting fluid: part I - flow and magnetic field

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003gapfd..97..429l&link_type=abstract

Geophysical and Astrophysical Fluid Dynamics, vol. 97, Issue 6, p.429-469

Physics

Fluid Dynamics

2

Scientific paper

The steady velocity, perturbation pressure and perturbation magnetic field, driven by an isolated buoyant parcel of Gaussian shape in a rapidly rotating, unconfined, incompressible electrically conducting fluid in the presence of an imposed uniform magnetic field, are obtained by means of the Fourier transform in the limit of small Ekman number. Lorentz and inertial forces are neglected. The solution requires at most evaluation of a single integral and is found in closed form in some spatial regions. The solution has structure on two disparate scales: on the scale of the buoyant parcel and on the scale of the Taylor column, which is elongated in the direction of the rotation axis. The detailed structures of the flow and pressure depend linearly on the relative orientation of gravity and rotation, with the solution for arbitrary orientation being a linear combination of two limiting cases in which these vectors are colinear (polar case) and perpendicular (equatorial case). The perturbation magnetic field depends additionally on the relative orientation of the imposed magnetic field, and three limiting cases of interest are presented in which gravity and rotation are colinear (polar-toroidal case), gravity and imposed field are colinear (equatorial-radial case) and all three are mutually perpendicular (equatorial-toroidal case). Visualization and analysis of the velocity and perturbation magnetic field vectors are facilitated by dividing these vector fields into geostrophic and ageostrophic protions. In all cases, the geostrophic and ageostrophic portions have different structure on the Taylor-column scale. The buoyancy force is balanced by a pressure force in the polar case and by a flux of momentum in the equatorial case. The pressure force and momentum flux do not decay in strength with increasing axial distance. Far from the parcel, the axial mass flux varies as the inverse one-third power of distance from the parcel. The velocity has a single geostrophic vortex in the polar case and two vortices in the equatorial case. The perturbation magnetic field has two, four and one geostrophic vortices in the polar-toroidal, equatorial-radial and equatorial-toroidal cases, respectively. To facilitate comparison of the present results with numerical simulations carried out in a finite domain, a set of boundary conditions are developed, with may be applied at a finite distance from the parcel.

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