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Plasma Flow and Solar Wind Acceleration in Non-Radial Coronal Magnetic Fields

Published online by Cambridge University Press:  04 August 2017

H. Biernat ,
N. Kömle  and
H. Rucker
H. Biernat
Affiliation:
Institut für Weltraumforschung, österreichische Akademie der Wissenschaften, Observatorium Lustbühel, Graz, Austria
N. Kömle
Affiliation:
Institut für Weltraumforschung, österreichische Akademie der Wissenschaften, Observatorium Lustbühel, Graz, Austria
H. Rucker
Affiliation:
Institut für Weltraumforschung, österreichische Akademie der Wissenschaften, Observatorium Lustbühel, Graz, Austria

Extract

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In the vicinity of the Sun — especially above coronal holes — the magnetic field lines show strong non-radial divergence and considerable curvature (see e.g. Kopp and Holzer, 1976; Munro and Jackson, 1977; Ripken, 1977). In the following we study the influence of these characteristics on the expansion velocity of the solar wind.

Type
V. Stellar Winds and Spindown in Late — Type Stars
Information
Symposium - International Astronomical Union , Volume 102: Solar and Stellar Magnetic Fields: Origins and Coronal Effects , 1983 , pp. 473 - 477
Copyright
Copyright © Reidel 1983 

References

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