The three-dimensional extent of a high speed solar wind stream |
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| Authors: | R J Macdowall M D Desch M L Kaiser R G Stone R A Hess A Balogh S J Bame B E Goldstein |
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| Institution: | (1) Code 695, NASA/GSFC, 20771 Greenbelt, MD, USA;(2) Hughes STX, 20706 Lanham, MD, USA;(3) The Blackett Laboratory, Imperial College, SW7 2BZ London, UK;(4) Los Alamos National Laboratory, 87545 Los Alamos, NM, USA;(5) Jet Propulsion Laboratory, 91109 Pasadena, CA, USA |
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| Abstract: | 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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