Solar-cycle evolution of the coronal general magnetic field of 1959?1974 and the synchronous variation of high-speed solar wind streams and galactic cosmic rays

Solar Physics ◽  
1977 ◽  
Vol 54 (1) ◽  
pp. 229-258 ◽  
Author(s):  
Hirokazu Yoshimura
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Cycle ◽  
Cosmic Rays ◽  
High Speed ◽  
Galactic Cosmic Rays ◽  
General Magnetic Field ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

scholarly journals Quasi-periodic changes in the 3D solar anisotropy of Galactic cosmic rays for 1965–2014

2017 ◽  
Vol 609 ◽  
pp. A32 ◽  
Author(s):  
R. Modzelewska ◽  
M. V. Alania
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Activity ◽  
Solar Cycle ◽  
Cosmic Rays ◽  
Ecliptic Plane ◽  
Galactic Cosmic Rays ◽  
Magnetic Cycle ◽  
The North ◽  
Solar Magnetic Cycle

Aims. We study features of the 3D solar anisotropy of Galactic cosmic rays (GCR) for 1965−2014 (almost five solar cycles, cycles 20−24). We analyze the 27-day variations of the 2D GCR anisotropy in the ecliptic plane and the north-south anisotropy normal to the ecliptic plane. We study the dependence of the 27-day variation of the 3D GCR anisotropy on the solar cycle and solar magnetic cycle. We demonstrate that the 27-day variations of the GCR intensity and anisotropy can be used as an important tool to study solar wind, solar activity, and heliosphere. Methods. We used the components Ar, Aϕ and At of the 3D GCR anisotropy that were found based on hourly data of neutron monitors (NMs) and muon telescopes (MTs) using the harmonic analyses and spectrographic methods. We corrected the 2D diurnal (~24-h) variation of the GCR intensity for the influence of the Earth magnetic field. We derived the north-south component of the GCR anisotropy based on the GG index, which is calculated as the difference in GCR intensities of the Nagoya multidirectional MTs. Results. We show that the behavior of the 27-day variation of the 3D anisotropy verifies a stable long-lived active heliolongitude on the Sun. This illustrates the usefulness of the 27-day variation of the GCR anisotropy as a unique proxy to study solar wind, solar activity, and heliosphere. We distinguish a tendency of the 22-yr changes in amplitude of the 27-day variation of the 2D anisotropy that is connected with the solar magnetic cycle. We demonstrate that the amplitudes of the 27-day variation of the north-south component of the anisotropy vary with the 11-yr solar cycle, but a dependence of the solar magnetic polarity can hardly be recognized. We show that the 27-day recurrences of the GG index and the At component are highly positively correlated, and both are highly correlated with the By component of the heliospheric magnetic field.

A Complete Catalogue of High-Speed Solar Wind Streams during Solar Cycle 23

Solar Physics ◽  
2013 ◽  
Vol 289 (3) ◽  
pp. 995-1012 ◽  
Author(s):  
G. Xystouris ◽  
E. Sigala ◽  
H. Mavromichalaki
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
High Speed ◽  
Solar Cycle 23 ◽  
Speed Solar Wind ◽  
Complete Catalogue ◽  
High Speed Solar Wind

scholarly journals Global thermospheric density variations caused by high-speed solar wind streams during the declining phase of solar cycle 23

2008 ◽  
Vol 113 (A11) ◽  
pp. n/a-n/a ◽  
Author(s):  
Jiuhou Lei ◽  
Jeffrey P. Thayer ◽  
Jeffrey M. Forbes ◽  
Eric K. Sutton ◽  
R. Steven Nerem ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
High Speed ◽  
Solar Cycle 23 ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

High Speed Solar Wind Forecast Model from the Solar Surface to 1AU Using Global 3D MHD Simulation

2017 ◽  
Vol 13 (S335) ◽  
pp. 272-275
Author(s):  
Mitsue Den ◽  
Takashi Tanaka ◽  
Yuki Kubo ◽  
Shinichi Watari
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
High Speed ◽  
Weather Forecasting ◽  
Solar Surface ◽  
Wind Condition ◽  
Geomagnetic Disturbances ◽  
Mhd Simulation ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

AbstractEmanating from coronals holes (CHs), high speed streams (HSSs) cause recurrent geomagnetic disturbances in the Earth’s magnetosphere. For this reason being able to predict the occurrence and timing of the high speed solar wind is one of the more important issues in space weather forecasting. Currently, it is still difficult to estimate the effect of a CH in case that it extends from high latitudes to lower ones. To monitor the global solar wind condition we have therefore developed a three-dimensional MHD simulation code, the REProduce Plasma Universe (REPPU) code, that is driven by the solar magnetic field from the solar surface to 1AU. The connectivity of magnetic field lines from CHs to Earth’s orbit via HSSs has been investigated. Simulation results are presented and the usefulness of our model is discussed.

Solar cycle evolution of high-speed solar wind streams

1976 ◽  
Vol 207 ◽  
pp. 977 ◽  
Author(s):  
S. J. Bame ◽  
J. R. Asbridge ◽  
W. C. Feldman ◽  
J. T. Gosling
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
High Speed ◽  
Speed Solar Wind ◽  
High Speed Solar Wind
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