Abstract
In this paper, we briefly review the experimental knowledge gained in the recent years on the interplanetary response to solar long-time scale phenomena such as the coronal magnetic structure and its evolution. Observational evidence that solar wind flow in the outer corona comes from the unipolar diverging magnetic regions of the photosphere is discussed along with relations to coronal holes. High-speed solar wind streams observed within the boundary of interplanetary magnetic sectors are associated with these structures. Their boundaries appear as very narrow velocity shears.
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D’Uston, C., Bosqued, J.M. (1980). Interplanetary Response to Solar Long Time-Scale Phenomena. In: Dryer, M., Tandberg-Hanssen, E. (eds) Solar and Interplanetary Dynamics. International Astronomical Union / Union Astronomique Internationale, vol 91. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9100-2_15
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DOI: https://doi.org/10.1007/978-94-009-9100-2_15
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