Propagation of a quasi bi-annual impulse close to the moment of the solar magnetic field polarity changing

Solar Physics ◽  
1995 ◽  
Vol 156 (2) ◽  
pp. 221-228 ◽  
Author(s):  
M. Sh. Gigolashvili ◽  
D. R. Japaridze ◽  
A. D. Pataraya ◽  
T. V. Zaqarashvili
Keyword(s):  
Magnetic Field ◽  
Solar Magnetic Field ◽  
Field Polarity ◽  
The Moment

Solar Differential Rotation at the Moment of Polarity Reversal of the Solar Magnetic Field

Astrophysics ◽  
2014 ◽  
Vol 57 (2) ◽  
pp. 296-303 ◽  
Author(s):  
M. Sh. Gigolashvili ◽  
D. R. Japaridze ◽  
B. B. Chargeishvili
Keyword(s):  
Magnetic Field ◽  
Differential Rotation ◽  
Solar Magnetic Field ◽  
Polarity Reversal ◽  
Solar Differential Rotation ◽  
The Moment

Generation of waves by the solar magnetic field polarity reversal

Solar Physics ◽  
1995 ◽  
Vol 157 (1-2) ◽  
pp. 31-44 ◽  
Author(s):  
A. D. Pataraya ◽  
T. V. Zaqarashvili
Keyword(s):  
Magnetic Field ◽  
Solar Magnetic Field ◽  
Polarity Reversal ◽  
Field Polarity

scholarly journals Influence of the asymmetry of the solar magnetic field polarity reversal on geomagnetic activity

2020 ◽  
Vol 24 (1) ◽  
Author(s):  
O. A. Baran ◽  
M. M. Koval'chuk ◽  
I. P. Laushnyk ◽  
M. I. Stodilka ◽  
M. B. Hirnyak
Keyword(s):  
Magnetic Field ◽  
Geomagnetic Activity ◽  
Solar Magnetic Field ◽  
Polarity Reversal ◽  
Field Polarity ◽  
The Asymmetry

THE DYNAMICS OF THE SOLAR MAGNETIC FIELD: POLARITY REVERSALS, BUTTERFLY DIAGRAM, AND QUASI-BIENNIAL OSCILLATIONS

2012 ◽  
Vol 749 (1) ◽  
pp. 27 ◽  
Author(s):  
A. Vecchio ◽  
M. Laurenza ◽  
D. Meduri ◽  
V. Carbone ◽  
M. Storini
Keyword(s):  
Magnetic Field ◽  
Solar Magnetic Field ◽  
Field Polarity ◽  
Polarity Reversals ◽  
Butterfly Diagram

scholarly journals Decay of turbulence in a liquid metal duct flow with transverse magnetic field

2019 ◽  
Vol 867 ◽  
pp. 661-690 ◽  
Author(s):  
Oleg Zikanov ◽  
Dmitry Krasnov ◽  
Thomas Boeck ◽  
Semion Sukoriansky
Keyword(s):  
Magnetic Field ◽  
Transverse Magnetic Field ◽  
Large Scale ◽  
High Amplitude ◽  
Transverse Magnetic ◽  
Duct Flow ◽  
Velocity Fluctuations ◽  
Turbulence Decay ◽  
The Moment ◽  
Typical Length

Decay of honeycomb-generated turbulence in a duct with a static transverse magnetic field is studied via direct numerical simulations. The simulations follow the revealing experimental study of Sukoriansky et al. (Exp. Fluids, vol. 4 (1), 1986, pp. 11–16), in particular the paradoxical observation of high-amplitude velocity fluctuations, which exist in the downstream portion of the flow when the strong transverse magnetic field is imposed in the entire duct including the honeycomb exit, but not in other configurations. It is shown that the fluctuations are caused by the large-scale quasi-two-dimensional structures forming in the flow at the initial stages of the decay and surviving the magnetic suppression. Statistical turbulence properties, such as the energy decay curves, two-point correlations and typical length scales are computed. The study demonstrates that turbulence decay in the presence of a magnetic field is a complex phenomenon critically depending on the state of the flow at the moment the field is introduced.

scholarly journals The Evolution of the Solar Magnetic Field

2012 ◽  
Vol 10 (H16) ◽  
pp. 86-89 ◽  
Author(s):  
J. Todd Hoeksema
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Solar Magnetic Field ◽  
Coronal Holes ◽  
Active Regions ◽  
Statistical Characteristics ◽  
Field Pattern ◽  
Small Scale ◽  
Polar Caps ◽  
Magnetic Elements

AbstractThe almost stately evolution of the global heliospheric magnetic field pattern during most of the solar cycle belies the intense dynamic interplay of photospheric and coronal flux concentrations on scales both large and small. The statistical characteristics of emerging bipoles and active regions lead to development of systematic magnetic patterns. Diffusion and flows impel features to interact constructively and destructively, and on longer time scales they may help drive the creation of new flux. Peculiar properties of the components in each solar cycle determine the specific details and provide additional clues about their sources. The interactions of complex developing features with the existing global magnetic environment drive impulsive events on all scales. Predominantly new-polarity surges originating in active regions at low latitudes can reach the poles in a year or two. Coronal holes and polar caps composed of short-lived, small-scale magnetic elements can persist for months and years. Advanced models coupled with comprehensive measurements of the visible solar surface, as well as the interior, corona, and heliosphere promise to revolutionize our understanding of the hierarchy we call the solar magnetic field.

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