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An estimate of solar wind velocity profiles in an coronal hole and a coronal streamer area (6-40 solar radius)Using the total electron content data obtained by the Ulysses Solar Corona Experiment during the superior solar conjunction in summer 1991, we selected two data sets, one associated with a coronal hole and the other one with coronal streamer crossings. By doing this data splitting, we find two entirely different density profiles varying as r(exp -2.7) and r(exp -2.3) for the coronal hole and coronal streamers, respectively. Assuming mass flux conservation from the inner corona to one AU, an estimate for the velocity profiles or acceleration in these two different regions can be determined. The more negative exponent of the coronal hole density profile indicates a more extended heating and acceleration region or more flaring, or both. Various possible explanations will be discussed.
Document ID
19960021470
Acquisition Source
Jet Propulsion Laboratory
Document Type
Conference Paper
Authors
Paetzold, M.
(Cologne Univ. Germany)
Tsurutani, B. T.
(Cologne Univ. Germany)
Bird, M. K.
(Cologne Univ. Germany)
Date Acquired
August 17, 2013
Publication Date
June 30, 1995
Subject Category
Solar Physics
Accession Number
96N24866
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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