Solar eruptions can produce effects that extend into the solar wind.
These effects are of three types: 1) ejecta containing solar matter and
magnetic fields, 2) the motion and redistribution of the ambient magnetic
field and plasma adjacent to the ejecta as a result of the interaction
between the ejecta and the solar wind, and 3) wave or shock disturbances
propagating away from the region of interaction. Magnetic clouds are the
simplest type of ejecta. Much progress has been made in recent years in
understanding magnetic clouds, and this work will be reviewed briefly.
Other types of ejecta, lacking a simple magnetic structure, are poorly
understood; some recent observations of these will be discussed. The flow
past ejecta and the interactions between ejecta and surrounding flows (including
other ejecta and shocks) can produce a multitude of configurations that
evolve with time. Some of the basic configurations will be reviewed. The
geometry and evolution of shocks produced by ejecta will also be discussed.
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