Pressure and magnetic field-induced transport effects in Ni45.4Mn40In14.6 alloy

2021 ◽  
Author(s):  
Sergiy M Konoplyuk ◽  
Alexandr V Kolomiets ◽  
J Prokleska ◽  
Petr Proschek ◽  
Volodymyr Buturlim ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Transport Effects

scholarly journals Flux-cutting and flux-transport effects in type-II superconductor slabs in a parallel rotating magnetic field

2011 ◽  
Vol 37 (11) ◽  
pp. 947-956 ◽  
Author(s):  
R. Cortés-Maldonado ◽  
J. E. Espinosa-Rosales ◽  
A. F. Carballo-Sánchez ◽  
F. Pérez-Rodríguez
Keyword(s):  
Magnetic Field ◽  
Rotating Magnetic Field ◽  
Type Ii ◽  
Flux Transport ◽  
Type Ii Superconductor ◽  
Transport Effects

Anomalous transport effects on magnetic field profile in a motional current sheath

2001 ◽  
Author(s):  
M. E. Kayama ◽  
E. A. Aramaki ◽  
R. P. Mota ◽  
M. A. Algatti ◽  
R. Y. Honda
Keyword(s):  
Magnetic Field ◽  
Anomalous Transport ◽  
Field Profile ◽  
Current Sheath ◽  
Magnetic Field Profile ◽  
Transport Effects

scholarly journals Point-contact spectroscopy of hopping transport: Effects of a magnetic field

2007 ◽  
Vol 75 (20) ◽  
Author(s):  
V. I. Kozub ◽  
A. A. Zyuzin ◽  
O. Entin-Wohlman ◽  
A. Aharony ◽  
Y. M. Galperin ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Point Contact ◽  
Hopping Transport ◽  
Point Contact Spectroscopy ◽  
Transport Effects

scholarly journals Toroidal models of magnetic field with twisted structure

2019 ◽  
Vol 5 (2) ◽  
pp. 69-75 ◽  
Author(s):  
Анастасия Петухова ◽  
Anastasia Petukhova ◽  
Станислав Петухов ◽  
Stanislav Petukhov
Keyword(s):  
Magnetic Field ◽  
Flux Rope ◽  
Forbush Decrease ◽  
Magnetic Clouds ◽  
Integral Model ◽  
Model Parameters ◽  
Magnetic Field Region ◽  
Transport Effects ◽  
Mass Ejection ◽  
The Magnetic Field

We present and discuss properties of the following magnetic field models in a magnetic cloud: Miller and Turner solution, modified Miller–Turner solution, Romashets–Vandas toroidal and integral models, and Krittinatham–Ruffolo model. Helicity of the magnetic field in all the models is the main feature of magnetic clouds. The first three models describe the magnetic field inside an ideal torus. In the integral model, parameters of a generating torus ambiguously determine the volume and form of the magnetic field region. In the Krittinatham–Ruffolo model, the cross-section radius of the torus is variable, thereby it corresponds more closely to the real form of magnetic clouds in the inner heliosphere. These models can be used to interpret in-situ observations of the magnetic flux rope, to study a Forbush decrease in magnetic clouds and transport effects of solar energetic particles injected into a coronal mass ejection.

scholarly journals Toroidal models of magnetic field with twisted structure

2019 ◽  
Vol 5 (2) ◽  
pp. 74-81
Author(s):  
Анастасия Петухова ◽  
Anastasia Petukhova ◽  
Станислав Петухов ◽  
Stanislav Petukhov
Keyword(s):  
Magnetic Field ◽  
Flux Rope ◽  
Forbush Decrease ◽  
Magnetic Clouds ◽  
Integral Model ◽  
Model Parameters ◽  
Magnetic Field Region ◽  
Transport Effects ◽  
Mass Ejection ◽  
The Magnetic Field

We present and discuss properties of the following magnetic field models in a magnetic cloud: Miller and Turner solution, modified Miller–Turner solution, Romashets–Vandas toroidal and integral models, and Krittinatham–Ruffolo model. Helicity of the magnetic field in all the models is the main feature of magnetic clouds. The first three models describe the magnetic field inside an ideal torus. In the integral model, parameters of a generating torus ambiguously determine the volume and form of the magnetic field region. In the Krittinatham–Ruffolo model, the cross-section radius of the torus is variable, thereby it corresponds more closely to the real form of magnetic clouds in the inner heliosphere. These models can be used to interpret in-situ observations of the magnetic flux rope, to study a Forbush decrease in magnetic clouds and transport effects of solar energetic particles injected into a coronal mass ejection.

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

Structure in the radiation of the galactic disk

1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Galactic Disk ◽  
Galactic Magnetic Field ◽  
Measured Polarization

Observations at various frequencies between 136 and 1400 MHz indicate a considerable amount of structure in the galactic disk. This result appears consistent both with measured polarization percentages and with considerations of the strength of the galactic magnetic field.

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