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The three-dimensional solar wind near solar minimum
A.R. Breen, D. Bisecker, A. Canals, R.A. Fallows, A. Lazarus, A. Lecinski,
Z. Mikic, P.J. Moran, B.J. Thompson and P.J.S. Williams
At solar minimum the heliosphere is dominated by fast solar wind from the
large coronal holes near the solar poles and slow wind above the streamer
belt, lying along the magnetic equator of the Sun. The magnetic equator is
inclined reletive to rotational equator of the Sun and is normally twisted,
so that fast streams can emerge close to the solar equator. In this
presentation we use interplanetary scintillation data from EISCAT in
conjunction with white-light measurements from SOHO and the Mauna Loa Solar
Observatory, extreme ultra-violet measurements from SOHO, solar
wind velocity measurements from Ulysses and Wind and coronal models to
study the three-dimensional solar wind. In particular, we consider the
emergence of streams of fast wind from equatorial coronal holes and the
variation of solar wind velocity across coronal hole boundaries.
(Paper presented by Prof. P.J.S. Williams (Cardiff)
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