Ulysses Solar Wind Plasma Observations at High Southerly Latitudes

Solar wind plasma observations made by the Ulysses spacecraft through -80.2° solar latitude and continuing equatorward to -40.1° are summarized. Recurrent high-speed streams and corotating interaction regions dominated at middle latitudes. The speed of the solar wind was typically 700 to 800 kilomet...

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Published inScience (American Association for the Advancement of Science) Vol. 268; no. 5213; pp. 1030 - 1033
Main Authors Phillips, J. L., Bame, S. J., Feldman, W. C., Goldstein, B. E., Gosling, J. T., Hammond, C. M., McComas, D. J., Neugebauer, M., Scime, E. E., Suess, S. T.
Format Journal Article
LanguageEnglish
Published Washington, DC American Society for the Advancement of Science 19.05.1995
American Association for the Advancement of Science
The American Association for the Advancement of Science
Subjects
Astronomical and space-research instrumentation
Astronomy
Coronal holes
Correlation
Earth, ocean, space
Electrons
Exact sciences and technology
Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations
Inferences
Interplanetary space
Lunar, planetary, and deep-space probes
Observations
Plasma astrophysics
Protons
Satellites
Scientific Concepts
Solar rotation
Solar system
Solar wind
Solar wind plasma
Spacecraft
Spectroheliographs
Sun
Sunspots
The Ulysses Mission
Topology
Tropical regions
Wind velocity
Heliosphere
Shock waves
Plasma
Ulysses space probes
Coronal mass ejection
Solar wind
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Summary:Solar wind plasma observations made by the Ulysses spacecraft through -80.2° solar latitude and continuing equatorward to -40.1° are summarized. Recurrent high-speed streams and corotating interaction regions dominated at middle latitudes. The speed of the solar wind was typically 700 to 800 kilometers per second poleward of -35°. Corotating reverse shocks persisted farther south than did forward shocks because of the tilt of the heliomagnetic streamer belt. Sporadic coronal mass ejections were seen as far south as -60.5°. Proton temperature was higher and the electron strahl was broader at higher latitudes. The high-latitude wind contained compressional, pressure-balanced, and Alfvenic structures.
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ISSN:0036-8075
1095-9203
DOI:10.1126/science.268.5213.1030