Solar Physics Division Meeting 2000, June 19-22
Session 1. Helioseismology, Magnetic Fields, Chromosphere and Transition Region
Display, Chair: C. U. Keller, Monday-Thursday, June 19, 2000, 8:00am-6:00pm, Forum Ballroom

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[1.35] 3D MHD Simulation of Flux Tube Dynamics: Comparison with Thin Flux Tube Models

G. H. Fisher, W. P. Abbett (UC Berkeley), Y. Fan (HAO/NCAR)

We have used the anelastic 3D MHD code ``ANMHD'' to perform simulations of emerging magnetic flux tubes moving in a gravitationally stratified background model representing the solar convection zone. The MHD model is computed within a local Cartesian geometry, with Coriolis forces included, using the f-plane approximation.

The evolution of flux tubes computed with the code will be compared and contrasted with results computed with the thin flux tube approximation.

This work was supported by NASA and NSF.

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