Turbulent Magnetic Transport Effects and their Relation to Magnetic Field Intermittency

1994 ◽  
pp. 311-320 ◽  
Author(s):  
S.I. Vainshtein ◽  
L. Tao ◽  
F. Cattaneo ◽  
R. Rosner
Keyword(s):  
Magnetic Field ◽  
Transport Effects ◽  
Magnetic Transport

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 On MHD rotational transport, instabilities and dynamo action in stellar radiation zones

2008 ◽  
Vol 4 (S259) ◽  
pp. 421-422
Author(s):  
Stéphane Mathis ◽  
A.-S. Brun ◽  
J.-P. Zahn
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
High Resolution ◽  
Magnetic Fields ◽  
Transport Processes ◽  
Dynamo Action ◽  
Mhd Instability ◽  
Mhd Simulations ◽  
Stellar Radiation ◽  
Magnetic Transport

AbstractMagnetic field and their related dynamical effects are thought to be important in stellar radiation zones. For instance, it has been suggested that a dynamo, sustained by a m = 1 MHD instability of toroidal magnetic fields (discovered by Tayler in 1973), could lead to a strong transport of angular momentum and of chemicals in such stable regions. We wish here to recall the different magnetic transport processes present in radiative zone and show how the dynamo can operate by recalling the conditions required to close the dynamo loop (BPol → BTor → BPol). Helped by high-resolution 3D MHD simulations using the ASH code in the solar case, we confirm the existence of the m = 1 instability, study its non-linear saturation, but we do not detect, up to a magnetic Reylnods number of 105, any dynamo action.

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 On MHD rotational transport, instabilities and dynamo action in stellar radiation zones

2008 ◽  
Vol 4 (S252) ◽  
pp. 255-256
Author(s):  
S. Mathis ◽  
J.-P. Zahn ◽  
A.-S. Brun
Keyword(s):  
Magnetic Field ◽  
Stellar Evolution ◽  
Dynamical Process ◽  
Transport Mechanisms ◽  
Dynamo Action ◽  
Mixing Processes ◽  
Mhd Instability ◽  
Stellar Radiation ◽  
Magnetic Transport ◽  
Transport And Mixing

AbstractMagnetic field is an essential dynamical process in stellar radiation zones. Moreover, it has been suggested that a dynamo action, sustained by a MHD instability which affects the toroidal axisymmetric magnetic field, could lead to a strong transport of angular momentum and of chemicals in such regions. Here, we recall the different magnetic transport and mixing processes in radiative regions. Next, we show that the dynamo cannot operate as described by Spruit (2002) and recall the condition required to close the dynamo loop. We perform high-resolution 3D simulations with the ASH code, where we observe indeed the MHD instability, but where we do not detect any dynamo action, contrary to J. Braithwaite (2006). We conclude on the picture we get for magnetic transport mechanisms in radiation zones and the associated consequences for stellar evolution.

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.

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