Magnetostatic interactions between sub-micrometer patterned magnetic elements

2001 ◽  
Vol 37 (4) ◽  
pp. 2052-2054 ◽  
Author(s):  
J. Janesky ◽  
N.D. Rizzo ◽  
L. Savtchenko ◽  
B. Engel ◽  
J.M. Slaughter ◽  
...  
Keyword(s):  
Magnetic Elements ◽  
Magnetostatic Interactions

Influence of magnetostatic interactions on the magnetization reversal of patterned magnetic elements

2011 ◽  
Vol 109 (7) ◽  
pp. 07D354 ◽  
Author(s):  
Xioalu Yin ◽  
S. H. Liou ◽  
A. O. Adeyeye ◽  
S. Jain ◽  
Baoshan Han
Keyword(s):  
Magnetization Reversal ◽  
Magnetic Elements ◽  
Magnetostatic Interactions

scholarly journals A sorter for electrons based on magnetic elements

2021 ◽  
pp. 113287
Author(s):  
Giulio Pozzi ◽  
Paolo Rosi ◽  
Amir H. Tavabi ◽  
Ebrahim Karimi ◽  
Rafal E. Dunin-Borkowski ◽  
...  
Keyword(s):  
Magnetic Elements

High resolution observations of small-scale magnetic elements and interpretation

Solar Physics ◽  
1996 ◽  
Vol 164 (1-2) ◽  
pp. 303-310 ◽  
Author(s):  
F. Kneer ◽  
F. Stolpe
Keyword(s):  
High Resolution ◽  
Small Scale ◽  
Magnetic Elements

Rotation of the magnetic elements in polar regions on the Sun

2007 ◽  
Vol 328 (10) ◽  
pp. 1016-1019 ◽  
Author(s):  
E.E. Benevolenskaya
Keyword(s):  
Polar Regions ◽  
The Sun ◽  
Magnetic Elements

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.

Turbulent convective flows in the solar photospheric plasma

2015 ◽  
Vol 81 (5) ◽  
Author(s):  
A. Caroli ◽  
F. Giannattasio ◽  
M. Fanfoni ◽  
D. Del Moro ◽  
G. Consolini ◽  
...  
Keyword(s):  
Mean Square Displacement ◽  
Small Scale ◽  
Solar Photosphere ◽  
Distribution Analysis ◽  
Pixel Resolution ◽  
Convective Flows ◽  
Magnetic Elements ◽  
Highly Nonlinear ◽  
Convective Motions ◽  
Short Time

The origin of the 22-year solar magnetic cycle lies below the photosphere where multiscale plasma motions, due to turbulent convection, produce magnetic fields. The most powerful intensity and velocity signals are associated with convection cells, called granules, with a scale of typically 1 Mm and a lifetime of a few minutes. Small-scale magnetic elements (SMEs), ubiquitous on the solar photosphere, are passively transported by associated plasma flows. This advection makes their traces very suitable for defining the convective regime of the photosphere. Therefore the solar photosphere offers an exceptional opportunity to investigate convective motions, associated with compressible, stratified, magnetic, rotating and large Rayleigh number stellar plasmas. The magnetograms used here come from a Hinode/SOT uninterrupted 25-hour sequence of spectropolarimetric images. The mean-square displacement of SMEs has been modelled with a power law with spectral index ${\it\gamma}$. We found ${\it\gamma}=1.34\pm 0.02$ for times up to ${\sim}2000~\text{s}$ and ${\it\gamma}=1.20\pm 0.05$ for times up to ${\sim}10\,000~\text{s}$. An alternative way to investigate the advective–diffusive motion of SMEs is to look at the evolution of the two-dimensional probability distribution function (PDF) for the displacements. Although at very short time scales the PDFs are affected by pixel resolution, for times shorter than ${\sim}2000~\text{s}$ the PDFs seem to broaden symmetrically with time. In contrast, at longer times a multi-peaked feature of the PDFs emerges, which suggests the non-trivial nature of the diffusion–advection process of magnetic elements. A Voronoi distribution analysis shows that the observed small-scale distribution of SMEs involves the complex details of highly nonlinear small-scale interactions of turbulent convective flows detected in solar photospheric plasma.

Magnetostatic interactions in various magnetosome clusters

2013 ◽  
Vol 113 (2) ◽  
pp. 023907 ◽  
Author(s):  
N. A. Usov ◽  
M. L. Fdez-Gubieda ◽  
J. M. Barandiarán
Keyword(s):  
Magnetostatic Interactions

Dynamical Interaction of Solar Magnetic Elements and Granular Convection: Results of a Numerical Simulation

1998 ◽  
Vol 495 (1) ◽  
pp. 468-484 ◽  
Author(s):  
O. Steiner ◽  
U. Grossmann‐Doerth ◽  
M. Knolker ◽  
M. Schussler
Keyword(s):  
Numerical Simulation ◽  
Dynamical Interaction ◽  
Magnetic Elements
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