Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh43b..08l&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH43B-08
Physics
2134 Interplanetary Magnetic Fields, 2169 Solar Wind Sources, 7509 Corona, 7524 Magnetic Fields, 7835 Magnetic Reconnection (2723, 7526)
Scientific paper
A number of diverse observations indicate that at least a portion of the slow solar wind plasma must originate from regions that were at one time magnetically closed (e.g., within the helmet streamer belt). The release of this material could result from closed fields expanding outward, balanced by disconnection of previously open fields, or it could occur through interchange reconnection, where open field lines reconnect with previously closed field lines. The scarcity of evidence for disconnection in interplanetary measurements has led to the idea that reconfiguration of coronal fields must occur entirely through interchange reconnection (e.g. Fisk and Schwadron 2001 ApJ 560, 425). We have performed several time-dependent MHD simulations of coronal evolution in the presence of surface flows such as differential rotation and the motion of small bipoles. We find that all three processes (disconnection, interchange reconnection, and opening of previously closed loops) occur. We discuss the implications of our work for the origin of the slow solar wind. Research supported by NASA, NSF (through CISM and the Strategic Capabilities Program) and AFOSR.
Linker Jon A.
Lionello Roberto
Mikic Zoran
Riley Pete
Titov Viacheslav S.
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