Interplanetary Scintillation Observations of the High-Latitude Solar Wind

Details Interplanetary Scintillation Observations of the High-Latitude Solar Wind Interplanetary Scintillation Observations of the High-Latitude Solar Wind

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ssrv...72..211c&link_type=abstract

Space Science Reviews, Volume 72, Issue 1-2, pp. 211-222

Computer Science

21

Solar Wind, Plasma, Interplanetary Scintillation

Scientific paper

Until the ULYSSES spacecraft reached the polar regions of the solar wind, the only high-latitude measurements available were from indirect techniques. The most productive observations in regions of the solar wind between 5R &sun; and 200R &sun; have been the family of radio scattering techniques loosely referred to as Interplanetary Scintillation (IPS) (Coles, 1978). Useful observations can be obtained using a variety of radio sources, for example spacecraft beacons, planetary radar echoes and compact cosmic sources (quasars, active galactic nuclei, pulsars, galactic masers, etc.). However for measurement of the high-latitude solar wind cosmic sources provide the widest coverage and this review will be confined to such observations. IPS observations played a very important role in establishing that polar coronal holes (first observed in soft x-ray emission) were sources of fast solar wind streams which occasionally extend down to the equatorial region and are observed by spacecraft. Here I will review the IPS technique and show the variation of both the velocity and the turbulence level with latitude over the last solar cycle. I will also outline recent work and discuss comparisons that we hope to make between IPS and ULYSSES observations.

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