  We present several models of the magnetic structure of solar coronal mass
ejections (CMEs). First, we model CMEs as expanding force-free magnetic
structures. While keeping the internal magnetic field structure of the
stationary solutions, expansion leads to complicated internal velocities and
rotation, while the field structures remain force-free.
  Second, expansion of a CME can drive resistive dissipation within the CME
changing the ionization states of different ions. We fit in situ measurements
of ion charge states to the resistive spheromak solutions.
  Finally, we consider magnetic field structures of fully confined stable
magnetic clouds containing both toroidal and poloidal magnetic fields and
having no surface current sheets. Expansion of such clouds may lead to sudden
onset of reconnection events.
