Associating the Solar Wind Measured by Ulysses with its Source at the sun |
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Authors: | Woo Richard Rifai Habbal Shadia |
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Institution: | (1) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, 91109, U.S.A;(2) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, U.S.A;(3) University of Wales, Aberystwyth, U.K. and |
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Abstract: | Radio occultation, ultraviolet, and white-light measurements have expanded our knowledge of the morphology of density and
velocity in polar coronal holes, and made it possible to carry out the first systematic comparisons between the Ulysses solar wind measurements and quantitative white-light observations of the solar corona. This paper summarizes the rationale
and salient features of this new approach which has been used to relate the solar wind observed by Ulysses in 1993–1995 to the inner corona. The statistical characteristics (average, standard deviation, and autocorrelation function)
of the Ulysses density measurements of the fast wind are found to be mirrored in those of polarized brightness measurements of path-integrated
density made by the High Altitude Observatory (HAO) Mauna Loa K-coronagraph at 1.15 R
⊙. These results reinforce the conclusions from comparisons between measurements of the outer and inner corona. They show that
the polar coronal hole extends radially into the solar wind, and that sources of the fast wind are not limited to coronal
holes.
This revised version was published online in August 2006 with corrections to the Cover Date. |
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