Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0516a&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0516
Physics
2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2169 Sources Of The Solar Wind, 7511 Coronal Holes, 7524 Magnetic Fields
Scientific paper
We have recently found evidence [Arge et al., 2002] suggesting that, in addition to magnetic field expansion factor, solar wind speed is also influenced by the angular separation (at the photosphere) between an open field footpoint and its nearest coronal hole boundary. From this discovery, we have developed a new technique for empirically specifying solar wind flow speed near the Sun (~ 0.1 AU) using a set of three simple inter-linked coronal/solar wind models. A preliminary test of the technique, using daily updated polar field corrected Mount Wilson Solar Observatory photospheric field synoptic maps from 1995, has yielded encouraging results. In this paper, we present the results of a more comprehensive and rigorous evaluation of this new method, which is now tested over a much larger fraction of the solar cycle. We also present the results of a preliminary test of our new empirical method using the Odstrcil 3-D time-dependent MHD numerical code.
Arge Charles Nickolos
Mayer Leslie R.
Odstrcil Dusan
Pizzo Victor J.
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