Source region of high and low speed wind during the Spartan 201-05 flight

The large-scale coronal magnetic fields of the Sun are believed to play an important role in organizing the coronal plasma and channeling the high and low speed solar wind along the open magnetic field lines of the polar coro nal holes and the rapidly diverging field lines close to the current sheet regions, as has been observed by the instruments aboard the Ulysses spacecr aft from March 1992 to March 1997. We have performed a study of this phenom ena within the framework of a semi-empirical model of the coronal expansion and solar wind using Spartan, SOHO, and Ulysses observations during the qu iescent phase of the solar cycle. Key to this understanding is the demonstr ation that the white light coronagraph data can be used to trace out the to pology of the coronal magnetic field and then using the Ulysses data to fix the strength of the surface magnetic field of the Sun. As a consequence, i t is possible to utilize this semi-empirical model with remote sensing obse rvation of the shape and density of the solar corona and in situ data of ma gnetic field and mass flux to predict values of the solar wind at all latit udes through out the solar system. We have applied this technique to the ob servations of Spartan 201-05 on 1-2 November, 1998, SOHO and Ulysses during the rising phase of this solar cycle and speculate on what solar wind velo cities Ulysses will observe during its polar passes over the south and the north poles during September of 2000 and 2001. In order to do this the mode l has been generalized to include multiple streamer belts and co-located cu rrent sheets. The model shows some interesting new results.