The high-latitude solar wind near sunspot maximum

Details The high-latitude solar wind near sunspot maximum The high-latitude solar wind near sunspot maximum

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997georl..24.3141w&link_type=abstract

Geophysical Research Letters, Volume 24, Issue 24, p. 3141-3144

Physics

15

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Sources Of The Solar Wind

Scientific paper

We use an empirical relation between solar wind speed and coronal flux-tube expansion to predict what Ulysses might have seen had it flown over the solar poles during 1989-1991 instead of 1994-1996. The wind speed patterns, derived from solar magnetograph data, show the following characteristics: (1) high-speed streams having recurrence rates of 28-29 days and originating from midlatitude extensions of the polar coronal holes dominate the rising phase of the sunspot cycle (1987-1989) (2) the persistent high-speed polar wind disappears and low-speed wind is found at all latitudes during 1989-1990 (3) very fast, episodic ``polar jets'' are generated as active region fields surge to the poles at the time of polar field reversal (1990-1991). The wind speed patterns that Ulysses encounters during its second polar orbit are expected to show the same general characteristics.

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