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Some basic structures in planetary nebulae are modeled as self-organizedmagnetohydrodynamic (MHD) plasma configurations with radial flow. Theseconfigurations are described by time self-similar dynamics, where space andtime dependences of each physical variable are in separable form. Axisymmetrictoroidal MHD plasma configuration is solved under the gravitational field of acentral star of mass $M$. With an azimuthal magnetic field, this self-similarMHD model provides an equatorial structure in the form of an axisymmetric toruswith nested and closed toroidal magnetic field lines. In the absence of anazimuthal magnetic field, this formulation models the basic features of bipolarplanetary nebulae. The evolution function, which accounts for the timeevolution of the system, has a bounded and an unbounded evolution trackgoverned respectively by a negative and positive energy density constant $H$.

Magnetohydrodynamic Model of Equatorial Plasma Torus in Planetary Nebulae