Linear force-free magnetic fields for solar extrapolation and interpretation

1989 ◽  
Vol 69 ◽  
pp. 323 ◽  
Author(s):  
G. Allen Gary
Keyword(s):  
Magnetic Fields ◽  
Linear Force

A Test on Two Codes for Extrapolating Solar Linear Force-free Magnetic Fields

Solar Physics ◽  
2009 ◽  
Vol 260 (1) ◽  
pp. 109-124 ◽  
Author(s):  
Yiwei Li ◽  
Guoxiang Song ◽  
Junlin Li
Keyword(s):  
Magnetic Fields ◽  
Linear Force

scholarly journals Topological study of active region 11158

2013 ◽  
Vol 8 (S300) ◽  
pp. 479-480
Author(s):  
Jie Zhao ◽  
Hui Li ◽  
Etienne Pariat ◽  
Brigitte Schmieder ◽  
Yang Guo ◽  
...  
Keyword(s):  
Active Region ◽  
Magnetic Fields ◽  
Free Field ◽  
Three Dimensional ◽  
Projection Data ◽  
Solar Dynamics Observatory ◽  
Equal Area ◽  
Linear Force ◽  
Solar Dynamics ◽  
Force Free Field

AbstractWith the cylindrical equal area (CEA) projection data from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO), we reconstructed the three-dimensional (3D) magnetic fields in the corona, using a non-linear force-free field (NLFFF) extrapolation method every 12 minutes during five days, to calculate the squashing degree factor Q in the volume. The results show that this AR has an hyperbolic flux tube (HFT) configuration, a typical topology of quadrupole, which is stable even during the two large flares (M6.6 and X2.2 class flares).

scholarly journals Linear Force-free Magnetic Fields and Coronal Models

1989 ◽  
Vol 42 (3) ◽  
pp. 317 ◽  
Author(s):  
CJ Durrant
Keyword(s):  
Boundary Condition ◽  
Magnetic Fields ◽  
Helmholtz Equation ◽  
Normal Component ◽  
Coordinate Systems ◽  
Mathematical Properties ◽  
Cylindrical Coordinate ◽  
Linear Force ◽  
Free Fields

The mathematical properties of linear force-free fields generated by the Helmholtz equation are reviewed, and the solutions in terms of spherical, cartesian and cylindrical coordinate systems are discussed. When only the normal component of the field on a single (photospheric) surface is available as a boundary condition, the solutions are not niquely determined. If further conditions are imposed, solutions may be unique or multiple or may not exist. The

scholarly journals Force-Free Models of Filament Channels

1998 ◽  
Vol 167 ◽  
pp. 274-277
Author(s):  
A.W. Longbottom
Keyword(s):  
Magnetic Fields ◽  
Multigrid Method ◽  
Flux Distribution ◽  
Free Field ◽  
Idealized Model ◽  
System A ◽  
Filament Channel ◽  
Linear Force ◽  
Field Lines ◽  
Force Free Field

AbstractA fast multigrid method to calculate the linear force-free field for a prescribed photospheric flux distribution is outlined. This is used to examine an idealized model of a filament channel. The magnetic fields, for a number of different field strengths and positions, are calculated and the height up to which field lines connect along the channel is examined. This is shown to strongly depend on the value of the helicity of the system. A possible explanation, in terms of the global helicity of the system, is suggested for the dextral/sinistral hemispheric pattern observed in filament channels.

scholarly journals Knotted linear force-free magnetic fields-topological aspects

PAMM ◽  
2007 ◽  
Vol 7 (1) ◽  
pp. 1026303-1026304
Author(s):  
P. Robert Kotiuga
Keyword(s):  
Magnetic Fields ◽  
Linear Force

Stability of force-free magnetic fields versus magnetic pitch

2002 ◽  
Vol 67 (2-3) ◽  
pp. 139-147
Author(s):  
Y. Q. HU ◽  
L. LI
Keyword(s):  
Magnetic Fields ◽  
Free Field ◽  
Plasma Phys ◽  
One Dimensional ◽  
Nonlinear Force ◽  
Linear Force ◽  
Free Fields ◽  
The Stability ◽  
Lowest Eigenvalue ◽  
Force Free Field

Starting from the one-dimensional energy integral and related stability theorems given by Newcomb [Ann. Phys (NY)10, 232 (1960)] for a linear pinch system, this paper analyses the stability of one-dimensional force-free magnetic fields in cylindrical coordinates (r, θ, z). It is found that the stability of the force-free field is closely related to the radial distribution of the pitch of the field lines: h(r) = 2πrBz/Bθ. The following three types of force-free fields are proved to be unstable: (i) force-free fields with a uniform pitch; (ii) force-free fields with a pitch that increases in magnitude with r in the neighbourhood of r = 0(d[mid ]h[mid ]/dr > 0); and (iii) force-free fields for which (dh/dr)r=0 = 0, Bθ α rm in the neighbourhood of r = 0, and (h d2h/dr2)r=0 > −128π2/(2m+4)2. On the other hand, the stability does not have a definite relation to the maximum of the force-free factor α defined by [dtri ]×B = αB. Examples will be given to illustrate that force-free fields with an infinite force-free factor at the boundary are stable, whereas those with a force-free factor that is finite and smaller than the lowest eigenvalue of linear force-free field solutions in the domain of interest are unstable. The latter disproves the sufficient criterion for stability of nonlinear force-free magnetic fields given by Krüger [J. Plasma Phys.15, 15 (1976)] that a nonlinear force-free field is stable if the maximum absolute value of the force-free factor is smaller than the lowest eigenvalue of linear force-free field solutions in the domain of interest.

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