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Session 14 - Solar-Terrestrial, Solar Wind.
Oral session, Monday, June 30
Ballroom A, Chair: David Webb
Due to the interplay of the differential rotation of the photosphere and the rigid rotation of the corona, the footpoints of heliospheric magnetic field lines move in latitude. In order to preserve \nabla \bfB = 0, one is forced into a reconnection process in low heliomagnetic latitudes. Such reconnection can provide an explanation for the origin of the slow solar wind.
We examine the properties of the solar wind generated by this diffusion reconnection process. We discuss implications for the large scale structure of the solar corona and the structure of coronal holes. We also show that this process naturally exhibits the charge state distributions observed with SWICS on Ulysses. We can also account for the observed overabundance of elements with low first ionization potential (the so-called FIP effect) in the slow solar wind, and its absence in fast, coronal hole associated wind. We also explore the dynamics of the low corona and the acceleration of the solar wind originating in this reconnection scenario.
Program listing for Monday