Three-dimensional structure of the coronal magnetic field and the solar wind speed distribution projected on the photosphere in 1974

AbstractWe have found correlated variations of the yearly averaged north-south asymmetry in the polar solar wind speed (Δsol) and the ratio of the zonal quadrupolar to the zonal dipolar contribution in the inferred coronal magnetic field during the declining phase of sunspot cycle 21. A physically meaningful association between Δsol and some polar solar magnetic field proxies is also observed during the low sunspot activity periods of the above cycle.

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Three-dimensional density and compressible magnetic structure in solar wind turbulence

Annales Geophysicae ◽

10.5194/angeo-36-527-2018 ◽

2018 ◽

Vol 36 (2) ◽

pp. 527-539 ◽

Cited By ~ 6

Author(s):

Owen W. Roberts ◽

Yasuhito Narita ◽

C.-Philippe Escoubet

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Three Dimensional ◽

Field Direction ◽

Dimensional Structure ◽

Magnetic Field Direction ◽

Three Dimensional Structure ◽

Slow Wind ◽

Incompressible Turbulence ◽

The Magnetic Field

Abstract. The three-dimensional structure of both compressible and incompressible components of turbulence is investigated at proton characteristic scales in the solar wind. Measurements of the three-dimensional structure are typically difficult, since the majority of measurements are performed by a single spacecraft. However, the Cluster mission consisting of four spacecraft in a tetrahedral formation allows for a fully three-dimensional investigation of turbulence. Incompressible turbulence is investigated by using the three vector components of the magnetic field. Meanwhile compressible turbulence is investigated by considering the magnitude of the magnetic field as a proxy for the compressible fluctuations and electron density data deduced from spacecraft potential. Application of the multi-point signal resonator technique to intervals of fast and slow wind shows that both compressible and incompressible turbulence are anisotropic with respect to the mean magnetic field direction P⟂≫P∥ and are sensitive to the value of the plasma beta (β; ratio of thermal to magnetic pressure) and the wind type. Moreover, the incompressible fluctuations of the fast and slow solar wind are revealed to be different with enhancements along the background magnetic field direction present in the fast wind intervals. The differences in the fast and slow wind and the implications for the presence of different wave modes in the plasma are discussed. Keywords. Interplanetary physics (MHD waves and turbulence)

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Correlation between Expansion Rate of the Coronal Magnetic Field and Solar Wind Speed in a Solar Activity Cycle

Solar Physics ◽

10.1007/s11207-005-3304-7 ◽

2005 ◽

Vol 227 (2) ◽

pp. 387-399 ◽

Cited By ~ 7

Author(s):

Kazuyuki Hakamada ◽

Masayoshi Kojima ◽

Tomoaki Ohmi ◽

Munetoshi Tokumaru ◽

Ken’ichi Fujiki

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Solar Activity ◽

Wind Speed ◽

Solar Wind Speed ◽

Activity Cycle ◽

Solar Activity Cycle ◽

Coronal Magnetic Field ◽

Expansion Rate

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Relationship Between Solar-Wind Speed and Coronal Magnetic-Field Properties

Solar Physics ◽

10.1007/s11207-015-0742-8 ◽

2015 ◽

Vol 290 (9) ◽

pp. 2491-2505 ◽

Cited By ~ 16

Author(s):

Ken’ichi Fujiki ◽

Munetoshi Tokumaru ◽

Tomoya Iju ◽

Kazuyuki Hakamada ◽

Masayoshi Kojima

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Wind Speed ◽

Solar Wind Speed ◽

Coronal Magnetic Field

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Three-dimensional structure of magnetic field in the mixed-μ levitation system using bulk superconductors

IEEE Transactions on Applied Superconductivity ◽

10.1109/77.783462 ◽

1999 ◽

Vol 9 (2) ◽

pp. 980-983 ◽

Cited By ~ 32

Author(s):

Y. Fukasawa ◽

H. Ohsaki

Keyword(s):

Magnetic Field ◽

Three Dimensional ◽

Dimensional Structure ◽

Three Dimensional Structure ◽

Bulk Superconductors ◽

Levitation System

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