Three Dimensional Compressible Convection in Oblique Magnetic Fields
**Previous
abstract** **Next
abstract**

**Session 86 -- Solar Active Regions**
*Display presentation, Wednesday, 11, 1995, 9:20am - 6:30pm*

## [86.01] Three Dimensional Compressible Convection in Oblique Magnetic Fields

*N.E.Hurlburt (Lockheed Solar and Astrophysics Lab.), P.C.Matthews (University of Nottingham), M.R.E.Proctor (Cambridge University)*

Magnetoconvection in the Sun does not take place in the idealized
situation in which the imposed field is vertical or
horizontal. Instead fields in sunspots and other active region
features are inclined to the vertical, and so the system does not
possess the left-right symmetry that is a part of many analytical
and numerical studies. As a step towards the understanding of
convection in general field configurations, we consider the nonlinear
behavior of three-dimensional compressible convection in the presence
of a uniform, externally-imposed, oblique magnetic field and in a
rectangular geometry. As in previous two-dimensional simulations, we
find that all solutions take the form of traveling waves for angles of
obliquity $0< \phi < \pi/2$, although the convection cells possess
definite three-dimensional structures. The resulting traveling
patterns heighten the impression that many of the dynamics observed
within sunspot penumbra may be a consequence of magnetoconvection in oblique
fields.

This work was supported in part by NASA contracts NASW-4612 and
NAS8-3974 and Lockheed Independent Research Funds.

**Wednesday
program listing**