Large-Scale and Small-Scale Solar Wind Structures Formed during Interaction of Streams in the Heliosphere

The paper considers the classification of solar wind streams in magnetohydrodynamic parameters (MHD-types); combinations of proton speed, density, temperature, and magnetic field strength, in addition to the classical solar wind separation into high-speed streams from coronal holes, transient stream...

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Bibliographic Details
Published in:Cosmic research 2019, Vol.57 (1), p.18-28
Main Authors: Rodkin, D. G., Kaportseva, K. B., Lukashenko, A. T., Veselovsky, I. S., Slemzin, V. A., Shugay, Yu. S.
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics and Astroparticles
Astrophysics and Cosmology
Charged particles
Computational fluid dynamics
Coronal holes
Coronal mass ejection
Field strength
Fluid flow
Heliosphere
High speed
Magnetic fields
Magnetohydrodynamics
Parameters
Physics
Physics and Astronomy
Solar corona
Solar wind
Solar wind properties
Solar wind velocity
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Streams
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Summary:The paper considers the classification of solar wind streams in magnetohydrodynamic parameters (MHD-types); combinations of proton speed, density, temperature, and magnetic field strength, in addition to the classical solar wind separation into high-speed streams from coronal holes, transient streams of coronal mass ejections, and the slow solar wind from the streamer belt. Two classifications of solar wind properties were compared for the events in August 2010 and May 2011, when one could observe the interaction of two coronal mass ejections and a coronal mass ejection with a high-speed solar wind stream from the coronal hole, respectively. It is shown that the classical description of a large-scale structure of wind streams (the ion wind composition especially) in scales of hours and days allows one to determine the type and source of streams, whereas the MHD-parameters allow one to more accurately describe the small-scale structure (in minutes), especially in the cases of several streams interaction in the heliosphere. The detailed study of a small-scale structure of stream interaction regions provides the information required for developing MHD-models describing the processes of propagation and interaction of streams in the heliosphere and for predicting their geoefficiency.
ISSN:0010-9525
1608-3075
DOI:10.1134/S0010952519010088