scholarly journals Boundary Fitting Problems Associated with Coronal Magnetic Models

1974 ◽  
Vol 57 ◽  
pp. 89-91 ◽  
Author(s):  
Kenneth H. Schatten
Keyword(s):  
Magnetic Fields ◽  
Legendre Polynomial ◽  
Magnetic Monopole ◽  
Polynomial Fit ◽  
Coronal Magnetic Fields ◽  
Boundary Fitting

The calculation of coronal magnetic fields was first suggested by Gold (1958). Altschuler and Newkirk (1969) and Newkirk et al. (1968) used a Legendre polynomial fit to the photospheric observations of magnetic fields whereas Schatten (1968) with Wilcox and Ness (Schatten et al., 1969) use a magnetic monopole fit, first incorporated by Schmidt (1964).

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

FINITE ENERGY ONE-HALF MONOPOLE SOLUTIONS

2012 ◽  
Vol 27 (40) ◽  
pp. 1250233 ◽  
Author(s):  
ROSY TEH ◽  
BAN-LOONG NG ◽  
KHAI-MING WONG
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Topological Charge ◽  
Magnetic Monopole ◽  
Magnetic Charge ◽  
Finite Energy ◽  
Spatial Infinity ◽  
Yang Mills ◽  
The Magnetic Field

We present finite energy SU(2) Yang–Mills–Higgs particles of one-half topological charge. The magnetic fields of these solutions at spatial infinity correspond to the magnetic field of a positive one-half magnetic monopole at the origin and a semi-infinite Dirac string on one-half of the z-axis carrying a magnetic flux of [Formula: see text] going into the origin. Hence the net magnetic charge is zero. The gauge potentials are singular along one-half of the z-axis, elsewhere they are regular.

Thermal condensations in coronal magnetic fields

Solar Physics ◽  
1988 ◽  
Vol 115 (1) ◽  
pp. 61-80 ◽  
Author(s):  
A. Hood ◽  
U. Anzer
Keyword(s):  
Magnetic Fields ◽  
Coronal Magnetic Fields

scholarly journals Distinguishing between coronal cloud prominences and channel prominences and their associations with solar and stellar flares

2015 ◽  
Vol 11 (S320) ◽  
pp. 278-287
Author(s):  
Sara F. Martin ◽  
Oddbjorn Engvold ◽  
Yong Lin ◽  
Jacqueline Alves da Silva
Keyword(s):  
Magnetic Fields ◽  
Sunspot Number ◽  
Maximum Height ◽  
Stellar Flares ◽  
Curved Trajectories ◽  
Coronal Magnetic Fields ◽  
Coronal Rain

AbstractTo better understand the differences between coronal cloud prominences and channel prominences, we systematically identified and analyzed coronal cloud prominences recorded in SDO/AIA images at 304 Å from 2010 May 20 through 2012 April 28. For the 225 cases identified, their numbers vary directly with the sunspot number. Their durations are typically less than 3 days. Their most frequent maximum height is 90,000 + and - 10,000 km. We offer our hypothesis that many coronal cloud prominences originate from some of the mass of previously erupted filaments ejected high out of their filament channels; subsequently part of this mass falls and collects in leaky magnetic troughs among coronal magnetic fields which constrain the leaked mass to slowly drain downward along curved trajectories where it appears as coronal rain. Currently there is inadequate evidence for a convincing correspondence between either coronal cloud prominences or channel prominences with stellar prominences detected to date.

Pseudo-magnetic fields of strongly-curved graphene nanobubbles

2018 ◽  
Vol 32 (11) ◽  
pp. 1850137 ◽  
Author(s):  
Li-Chi Liu
Keyword(s):  
Magnetic Fields ◽  
Magnetic Monopole ◽  
Spherical Surface ◽  
Tight Binding ◽  
Constant Field ◽  
Curvature Effect ◽  
Tight Binding Model ◽  
Binding Model ◽  
The Magnetic Field ◽  
Orbital Axis

We use the [Formula: see text]-orbital axis vector (POAV) analysis to deal with large curvature effect of graphene in the tight-binding model. To test the validities of pseudo-magnetic fields (PMFs) derived from the tight-binding model and the model with Dirac equation coupled to a curved surface, we propose two types of spatially constant-field topographies for strongly-curved graphene nanobubbles, which correspond to these two models, respectively. It is shown from the latter model that the PMF induced by any spherical graphene nanobubble is always equivalent to the magnetic field caused by one magnetic monopole charge distributed on a complete spherical surface with the same radius. Such a PMF might be attributed to the isometry breaking of a graphene layer attached conformably to a spherical substrate with adhesion.

Coronal Magnetic Fields from Polarization Observations at Microwaves

1996 ◽  
pp. 443-444
Author(s):  
F. Chiuderi Drago ◽  
F. Borgioli ◽  
C. E. Alissandrakis ◽  
M. Hagyard ◽  
K. Shibasaki
Keyword(s):  
Magnetic Fields ◽  
Coronal Magnetic Fields
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