The Three-Dimensional Extent of a High-Speed Solar Wind Stream

Details The Three-Dimensional Extent of a High-Speed Solar Wind Stream The Three-Dimensional Extent of a High-Speed Solar Wind Stream

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ssrv...72..125m&link_type=abstract

Space Science Reviews, Volume 72, Issue 1-2, pp. 125-128

Computer Science

4

Scientific paper

A primary goal of the Ulysses mission is to study the 3-dimensional structures making up the interplanetary medium, and example of which is the high speed solar wind stream observedin situ by Ulysses beginning in July 1992. In order to study the longitudinal extent of this stream as a function of Ulysses' increasing heliographic latitude, a second point of reference is required to separate spatial and temporal variations. Such a reference point is provided at Jupiter by a class of Jovian radio bursts, whose occurrence rate varies in a predictable way with solar wind speed. Using thein situ and remote observations from Ulysses, the extent of the high speed stream at ˜5 AU is mapped and compared to the associated coronal hole boundary on the Sun.

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