ULYSSES solar wind plasma observations from peak southerly latitude through perihelion and beyond

Details ULYSSES solar wind plasma observations from peak southerly latitude through perihelion and beyond ULYSSES solar wind plasma observations from peak southerly latitude through perihelion and beyond

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...44p&link_type=abstract

International Solar Wind 8 Conference, p. 44

Physics

Ulysses Mission, Solar Wind, Plasma Interactions, Perihelions, Shock Waves, Wind Velocity, Coronal Holes, Spacecraft Trajectories, Stellar Mass Ejection, Sun

Scientific paper

The Ulysses spacecraft trajectory includes a peak southern latitude of -80.2 deg, reached during September 1994, and perihelion in the ecliptic plane at 134 AU in March 1995. The near-perihelion mission phase features a rapid scan through solar latitude, with rates approaching one degree per day. We will present observations through mid-May 1995, when the spacecraft will be near 1.5 AU and +50 deg solar latitude. At the time of this writing, observations from the solar wind plasma experiment have been examined through -40 deg solar latitude. At that latitude Ulysses was still immersed in fast solar wind from the south polar coronal hole, with wind speeds of 700 to 800 km/s and with a variety of fine structure. Expectations for near-perihelion measurements include times of slow, dense wind characteristic of the near-equatorial heliomagnetic streamer belt. A non-zero tilt of the streamer belt would produce recurrent intervals of fast coronal hole wind and corotating interaction regions (CIRs) caused by fast wind overtaking slow wind. Forward and reverse shock waves bounding the CIRs, routinely observed at low and intermediate latitudes beyond approximately 2 AU, will likely be absent during the northward transit due to proximity to the Sun we will summarize solar wind plasma results concerning meridional gradients in fluid parameters, large-scale and fine structure, and transient events such as coronal mass ejections.

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