Background and Local Magnetic Fields on the Solar Surface

1994 ◽  
pp. 129-162
Author(s):  
Ye Shi-Hui
Keyword(s):  
Magnetic Fields ◽  
Solar Surface ◽  
Local Magnetic Fields

The Local Magnetic Fields Probed by µ+ in hcp Ferromagnets: Co and Gd

1978 ◽  
Vol 44 (4) ◽  
pp. 1131-1141 ◽  
Author(s):  
Nobuhiko Nishida ◽  
Kanetada Nagamine ◽  
Ryugo S. Hayano ◽  
Toshimitsu Yamazaki ◽  
D. G. Fleming ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Local Magnetic Fields

scholarly journals Correlations between charge ordering and local magnetic fields in overdopedYBa2Cu3O6+x

2002 ◽  
Vol 66 (13) ◽  
Author(s):  
J. E. Sonier ◽  
J. H. Brewer ◽  
R. F. Kiefl ◽  
R. H. Heffner ◽  
K. F. Poon ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Charge Ordering ◽  
Local Magnetic Fields

scholarly journals Quantum walks on graphs of the ordered Hamming scheme and spin networks

2019 ◽  
Vol 7 (1) ◽  
Author(s):  
Hiroshi Miki ◽  
Satoshi Tsujimoto ◽  
Luc Vinet
Keyword(s):  
Magnetic Fields ◽  
Quantum Walks ◽  
Perfect State ◽  
Spin Networks ◽  
Krawtchouk Polynomials ◽  
Energy Eigenstates ◽  
State Transfer ◽  
Perfect State Transfer ◽  
Local Magnetic Fields ◽  
Basis Vectors

It is shown that the hopping of a single excitation on certain triangular spin lattices with non-uniform couplings and local magnetic fields can be described as the projections of quantum walks on graphs of the ordered Hamming scheme of depth 2. For some values of the parameters the models exhibit perfect state transfer between two summits of the lattice. Fractional revival is also observed in some instances. The bivariate Krawtchouk polynomials of the Tratnik type that form the eigenvalue matrices of the ordered Hamming scheme of depth 2 give the overlaps between the energy eigenstates and the occupational basis vectors.

A Simulation Study of the Magnetic Reconnections Between Closed Loops and Open Magnetic Fields Driven by Horizontal Flows on Solar Surface

2014 ◽  
Vol 38 (1) ◽  
pp. 43-55
Author(s):  
CHEN Wen-lei ◽  
HE Jian-shen ◽  
WU S.T. ◽  
YANG Li-ping ◽  
WANG Ai-hua ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Simulation Study ◽  
Solar Surface ◽  
Closed Loops ◽  
Horizontal Flows

NQR determination of local magnetic fields in senarmonite (Sb2O3)

1996 ◽  
Vol 251 (3-4) ◽  
pp. 250-251 ◽  
Author(s):  
G.K. Semin ◽  
A.A. Boguslavsky
Keyword(s):  
Magnetic Fields ◽  
Local Magnetic Fields

scholarly journals Small-Scale Solar Magnetic Fields

1976 ◽  
Vol 71 ◽  
pp. 69-99 ◽  
Author(s):  
J. O. Stenflo
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Solar Surface ◽  
Life Time ◽  
Wave Number ◽  
Small Scale ◽  
Solar Magnetic Fields ◽  
Field Amplification ◽  
Wave Numbers ◽  
Diffuse Form

The observed properties of small-scale solar magnetic fields are reviewed. Most of the magnetic flux in the photosphere is in the form of strong fields of about 100–200 mT (1–2 kG), which have remarkably similar properties regardless of whether they occur in active or quiet regions. These fields are associated with strong atmospheric heating. Flux concentrations decay at a rate of about 107 Wb s-1, independent of the amount of flux in the decaying structure. The decay occurs by smaller flux fragments breaking loose from the larger ones, i.e. a transfer of magnetic flux from smaller to larger Fourier wave numbers, into the wave-number regime where ohmic diffusion becomes significant. This takes place in a time-scale much shorter than the length of the solar cycle.The field amplification occurs mainly below the solar surface, since very little magnetic flux appears in diffuse form in the photosphere, and the life-time of the smallest flux elements is very short. The observations further suggest that most of the magnetic flux in quiet regions is supplied directly from below the solar surface rather than being the result of turbulent diffusion of active-region magnetic fields.

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