Equilibrium Configurations of Magnetized Rotating Polytropes: Effects of Strong Toroidal Magnetic Fields in Addition to Poloidal Magnetic Fields

2006 ◽  
Vol 164 (1) ◽  
pp. 156-172 ◽  
Author(s):  
Shijun Yoshida ◽  
Yoshiharu Eriguchi
Keyword(s):  
Magnetic Fields ◽  
Equilibrium Configurations ◽  
Poloidal Magnetic Fields

The Distribution of Radio Polarisation in Three Southern Galaxies

1991 ◽  
Vol 9 (2) ◽  
pp. 266-268
Author(s):  
J. I. Harnett ◽  
U. Klein ◽  
R. Wielebinski ◽  
R. F. Haynes
Keyword(s):  
Cosmic Rays ◽  
Magnetic Fields ◽  
Radio Telescope ◽  
Spiral Galaxies ◽  
Total Power ◽  
Transport Mechanisms ◽  
Contour Plots ◽  
Preliminary Study ◽  
Poloidal Magnetic Fields

AbstractWe are studying the distribution and morphology of magnetic fields in southern face-on and edge-on galaxies with the intention of clarifying the distribution, lifetimes and transport mechanisms of cosmic rays, and investigating the intensity and orientation of the disc, halo and poloidal magnetic fields. As a preliminary study, before the Australia Telescope was available, we observed a sample of well-known southern spiral galaxies with the Parkes radio telescope.Here, we present the resulting polarisation images for three galaxies, NGC 253, M 83 and NGC 4945, which were observed at 4.75 GHz and 8.55 GHz. The corresponding total power contour plots have been already published by Harnett et al. (1989a, 1990).

The Toroidal and Poloidal Coil Systems of JET

1986 ◽  
Vol 200 (2) ◽  
pp. 81-94 ◽  
Author(s):  
J R Last
Keyword(s):  
Magnetic Fields ◽  
Design And Manufacture ◽  
Poloidal Magnetic Fields

This paper describes the design and manufacture of coils to produce the toroidal and poloidal magnetic fields of the JET (Joint European Torus) Tokamak fusion project.

Poloidal Magnetic Fields in Galactic Central Regions

1990 ◽  
pp. 394-394
Author(s):  
H. Lesch ◽  
A. Crusius-Wätzel ◽  
R. Schlickeiser ◽  
R. Wielebinski
Keyword(s):  
Magnetic Fields ◽  
Central Regions ◽  
Poloidal Magnetic Fields

scholarly journals Toroidal versus poloidal magnetic fields in Sun-like stars: a rotation threshold

2008 ◽  
Vol 388 (1) ◽  
pp. 80-88 ◽  
Author(s):  
P. Petit ◽  
B. Dintrans ◽  
S. K. Solanki ◽  
J.-F. Donati ◽  
M. Aurire ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Poloidal Magnetic Fields

scholarly journals Stationary and axisymmetric configurations of compact stars with extremely strong and highly localized magnetic fields

2010 ◽  
Vol 6 (S274) ◽  
pp. 232-235
Author(s):  
Kotaro Fujisawa ◽  
Shin'ichiro Yoshida ◽  
Yoshiharu Eriguchi
Keyword(s):  
Magnetic Fields ◽  
Current Density ◽  
Compact Stars ◽  
Model Parameters ◽  
Flux Function ◽  
Narrow Region ◽  
Deep Interior ◽  
Equilibrium Configurations ◽  
Basic Equations ◽  
New Formulation

AbstractUsing a new formulation to compute structures of stationary and axisymmetric magnetized barotropic stars in Newtonian gravity, we have succeeded in obtaining numerically exact models of stars with extremely high interior magnetic fields. In this formulation, there appear four arbitrary functions of the magnetic flux function from the integrability conditions among the basic equations. Since in our new formulation these arbitrary functions appear in the expression of the current density, configurations with different current distributions can be specified by choosing the forms of the arbitrary functions.By choosing appropriate forms for the four arbitrary functions, we have solved many kinds of equilibrium configurations both with poloidal and toroidal magnetic fields. Among them, by choosing special form for the toroidal current density, we have been able to obtain magnetized stars which have extremely strong poloidal magnetic fields deep inside the core region near the symmetric axis. By adopting the appropriate model parameters for the neutron stars, the magnetic fields could be 1014 ~ 1015 G on the surfaces and be about 1017 G in the deep interior regions. For other model parameters appropriate for white dwarfs, the magnetic fields could be around 107 ~ 108 G (surface regions) and 109 ~ 1010 G (core regions). It is remarkable that the regions with very strong interior magnetic fields are confined to a very narrow region around the symmetric axis in the central part of the stars. The issues of stability of these configurations and of evolutionary paths to reach such configurations need to be investigated in the future work.

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