Complete numerical description of nonlocal quantum diffusion in an array of magnetic-flux vortices

1994 ◽  
Vol 50 (23) ◽  
pp. 17621-17624 ◽  
Author(s):  
S. J. Bending
Keyword(s):  
Magnetic Flux ◽  
Quantum Diffusion ◽  
Nonlocal Quantum ◽  
Flux Vortices ◽  
Magnetic Flux Vortices

scholarly journals Extracting, Tracking, and Visualizing Magnetic Flux Vortices in 3D Complex-Valued Superconductor Simulation Data

2016 ◽  
Vol 22 (1) ◽  
pp. 827-836 ◽  
Author(s):  
Hanqi Guo ◽  
Carolyn L. Phillips ◽  
Tom Peterka ◽  
Dmitry Karpeyev ◽  
Andreas Glatz
Keyword(s):  
Magnetic Flux ◽  
Simulation Data ◽  
Flux Vortices ◽  
Magnetic Flux Vortices ◽  
Complex Valued

Video Tracks Motion of Magnetic Flux Vortices

Physics Today ◽  
1993 ◽  
Vol 46 (2) ◽  
pp. 20-20
Author(s):  
Barbara Goss Levi
Keyword(s):  
Magnetic Flux ◽  
Flux Vortices ◽  
Magnetic Flux Vortices

Transition from thermally activated to regular flow of magnetic flux vortices in HTSC

2000 ◽  
Vol 42 (9) ◽  
pp. 1596-1601
Author(s):  
V. N. Kushnir ◽  
A. Yu. Petrov ◽  
S. L. Prischepa
Keyword(s):  
Magnetic Flux ◽  
Thermally Activated ◽  
Flux Vortices ◽  
Magnetic Flux Vortices ◽  
Regular Flow

Emergence of Twisted Magnetic Flux Related Sigmoidal Brightening

2000 ◽  
Vol 179 ◽  
pp. 263-264
Author(s):  
K. Sundara Raman ◽  
K. B. Ramesh ◽  
R. Selvendran ◽  
P. S. M. Aleem ◽  
K. M. Hiremath
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Ultra Violet ◽  
Active Regions ◽  
Morphological Properties ◽  
Energy Storage And Conversion ◽  
The Sun ◽  
X Rays ◽  
The Magnetic Field

Extended AbstractWe have examined the morphological properties of a sigmoid associated with an SXR (soft X-ray) flare. The sigmoid is cospatial with the EUV (extreme ultra violet) images and in the optical part lies along an S-shaped Hαfilament. The photoheliogram shows flux emergence within an existingδtype sunspot which has caused the rotation of the umbrae giving rise to the sigmoidal brightening.It is now widely accepted that flares derive their energy from the magnetic fields of the active regions and coronal levels are considered to be the flare sites. But still a satisfactory understanding of the flare processes has not been achieved because of the difficulties encountered to predict and estimate the probability of flare eruptions. The convection flows and vortices below the photosphere transport and concentrate magnetic field, which subsequently appear as active regions in the photosphere (Rust & Kumar 1994 and the references therein). Successive emergence of magnetic flux, twist the field, creating flare productive magnetic shear and has been studied by many authors (Sundara Ramanet al.1998 and the references therein). Hence, it is considered that the flare is powered by the energy stored in the twisted magnetic flux tubes (Kurokawa 1996 and the references therein). Rust & Kumar (1996) named the S-shaped bright coronal loops that appear in soft X-rays as ‘Sigmoids’ and concluded that this S-shaped distortion is due to the twist developed in the magnetic field lines. These transient sigmoidal features tell a great deal about unstable coronal magnetic fields, as these regions are more likely to be eruptive (Canfieldet al.1999). As the magnetic fields of the active regions are deep rooted in the Sun, the twist developed in the subphotospheric flux tube penetrates the photosphere and extends in to the corona. Thus, it is essentially favourable for the subphotospheric twist to unwind the twist and transmit it through the photosphere to the corona. Therefore, it becomes essential to make complete observational descriptions of a flare from the magnetic field changes that are taking place in different atmospheric levels of the Sun, to pin down the energy storage and conversion process that trigger the flare phenomena.

Large-scale Motion of Solar Filaments

2000 ◽  
Vol 179 ◽  
pp. 205-208
Author(s):  
Pavel Ambrož ◽  
Alfred Schroll
Keyword(s):  
Magnetic Flux ◽  
Proper Motion ◽  
Time Scale ◽  
Large Scale ◽  
Accuracy Of Measurements ◽  
Solar Filaments ◽  
General Movement ◽  
Scale Motion ◽  
Velocity Scatter

AbstractPrecise measurements of heliographic position of solar filaments were used for determination of the proper motion of solar filaments on the time-scale of days. The filaments have a tendency to make a shaking or waving of the external structure and to make a general movement of whole filament body, coinciding with the transport of the magnetic flux in the photosphere. The velocity scatter of individual measured points is about one order higher than the accuracy of measurements.

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