The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
|Number of pages
|Comparative Reconnection Studies at the Sun and in Planetary Magnetospheres
|Published - 2002