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Two Classes of Fast Solar Wind Streams: Their Origin and Influence on the Galactic Cosmic Ray Intensity

Published online by Cambridge University Press:  14 August 2015

N. Iucci ,
M. Parisi ,
M. Storini  and
G. Villoresi
N. Iucci
Affiliation:
Istituto di Fisica dell'Università Laboratorio Plasma Spazio del C.N.R. Piazzale delle Scienze, 5 - 00185 Roma, Italy
M. Parisi
Affiliation:
Istituto di Fisica dell'Università Laboratorio Plasma Spazio del C.N.R. Piazzale delle Scienze, 5 - 00185 Roma, Italy
M. Storini
Affiliation:
Istituto di Fisica dell'Università Laboratorio Plasma Spazio del C.N.R. Piazzale delle Scienze, 5 - 00185 Roma, Italy
G. Villoresi
Affiliation:
Istituto di Fisica dell'Università Laboratorio Plasma Spazio del C.N.R. Piazzale delle Scienze, 5 - 00185 Roma, Italy

Extract

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The analysis of solar wind (bulk velocity v, proton density n, proton temperature T) and magnetic field (B) data in the years 1964-1974 makes possible to identify two main classes of high-speed streams (ΔV = (vm - vo)≥ 100 km/sec, vm being the maximum daily mean speed and vo the mean value between the speeds immediately preceding and following the stream; duration Δt ≥ 2 days):

Type
Part V. Coronal and Interplanetary Responses to Short Time Scale Phenomena: - Observations
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 399 - 401
Copyright
Copyright © Reidel 1980 

References

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