Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm54a..05t&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SM54A-05
Physics
2706 Cusp, 2716 Energetic Particles: Precipitating, 2723 Magnetic Reconnection (7526, 7835)
Scientific paper
The location of the reconnection line in relation to regions where accelerated plasma flows have been reported with local magnetic shear angles greater than 50° greatly influences the mass and energy transfer from the solar wind to the magnetosphere. The highest transfer rates are achieved for conditions where the merging fields are anti-parallel. Recent studies concerning the location of the reconnection line with single point measurements under stable solar wind and IMF conditions reveal that the so-called tilted X-line, crossing the dayside sub-solar region, is the dominant reconnection scenario. Magnetic reconnection tends to occur along a continuous X-line of maximum magnetic shear across the dayside magnetopause. Exceptions to this reconnection location are dominant southward IMF conditions (within ±25° of southward IMF) or a dominant IMF Bx component (more than 70% of the IMF in the Bx component) for which the reconnection line bifurcates, and exists along magnetopause regions where the merging fields are exactly anti-parallel. In this presentation we will discuss specific exceptions and differences to the statistical reconnection location model determined from times of stable and unchanged IMF conditions. These differences are most probably caused by the dynamic nature of the IMF direction. Reconnection locations during slow changing IMF clock angles show a certain reluctance to adjust to the new conditions of the changing field and show locations of earlier IMF conditions. An additional puzzling feature is the occurrence of reconnection location anomalies around an IMF clock angle of about 230°.
Fuselier Stephen A.
Petrinec Steven M.
Trattner K. J.
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