Image Details
Caption: Fig. 5.
Dynamics associated with the nonstatic equilibrium achieved for case M1, shown at ﹩t=6.7﹩ (and at an arbitrary x, since the fields are x‐invariant). Left: (y, z) cross section of the domain, with shading representing density perturbation (dark is negative) and arrows indicating the (﹩v﹩, w) flow. Right: Volume rendering of B2. A density deficit can clearly be seen where the magnetic structures exist, and the poloidal flow driven by the resulting buoyancy forces is apparent.
© 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A.