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In Situ Observations and Interpretations of Solar Eruptions

Leonard Burlaga


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.

  Organization: NASA/GSFC
     Telephone: 301-286-5956
           Fax: 301-286-1683
        e-mail: burlaga@lepvax.gsfc.nasa.gov
       Address: NASA/GSFC
   Code 692
   Greenbelt, MD 20771

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