Evolution of the Magnetic Field Configuration in an Active Region

1971 ◽  
pp. 243-248
Author(s):  
Dennis L. Schatz
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Field Configuration ◽  
Magnetic Field Configuration ◽  
The Magnetic Field

scholarly journals Evolution of the Magnetic Field Configuration in an Active Region

1971 ◽  
Vol 43 ◽  
pp. 243-248 ◽  
Author(s):  
Dennis L. Schatz
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Time Resolution ◽  
Field Configuration ◽  
High Time ◽  
High Time Resolution ◽  
Magnetic Field Configuration ◽  
The Magnetic Field

Described and discussed is the evolution of the magnetic field configuration in an Active Region from observations made with high time resolution.

scholarly journals Sunspot Proper Motion and Flare Frequency

1995 ◽  
Vol 151 ◽  
pp. 45-46
Author(s):  
G. Csepura ◽  
L. Győri ◽  
A.A. Galal
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Proper Motion ◽  
Active Regions ◽  
Field Configuration ◽  
Flare Activity ◽  
Magnetic Field Configuration ◽  
Spot Group ◽  
The Magnetic Field ◽  
Flare Frequency

Flare activity of solar active regions is generally believed to depend on a sheared configuration of magnetic fields (Hagyard et al. 1984). There are cases when the shear necessary for a flare can be attributed to the emergence of a new flux in the spot group (Wang 1992). But, perhaps, a newly born active region can also influence the magnetic field configuration in a nearby active region (Poleto et al. 1993, Gesztelyi et al. 1993). In this paper we are interested primarily in the influence of a newly emerging spot group on a nearby one.The three neighbouring active regions NOAA AR 6412(B-C), 6413(A) and 6415(D) have been studied between 13-22 December 1990. White-light pictures for studying sunspot proper motion and area evolution were taken at Gyula Observing Station (Hungary), Debrecen Heliophysical Observatory (Hungary) and Helwan Observatory (Egypt). Times and positions of the flares were taken from the Solar Geophysical Data (No. 558, part 1, February 1991).

Description of the magnetic field configuration near the boundary of the geomagnetic tail

1981 ◽  
Vol 1 (1) ◽  
pp. 239-242
Author(s):  
D. Teodosiev ◽  
I. Konstantinov
Keyword(s):  
Magnetic Field ◽  
Field Configuration ◽  
Magnetic Field Configuration ◽  
Geomagnetic Tail ◽  
The Magnetic Field

scholarly journals Magnetic Field Configuration in 4C 39.25

1998 ◽  
Vol 164 ◽  
pp. 115-116 ◽  
Author(s):  
A. Alberdi ◽  
L. Lara ◽  
J.L. Gómez ◽  
J.M. Marcaide ◽  
M.A. Pérez-Torres ◽  
...  
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Radio Emission ◽  
Field Configuration ◽  
Radio Sources ◽  
Magnetic Field Configuration ◽  
Relativistic Jet ◽  
Scale Structures ◽  
The Magnetic Field

AbstractWe have performed simultaneous multi-frequency polarization VLBA observations of the compact radio sources 3C 395 and 4C 39.25 which show both stationary and superluminal components in their parsec-scale structures. Those of 3C 395 have been reported elsewhere. Here we report on high resolution maps of the total intensity and polarized radio emission of 4C 39.25, trace the magnetic field configuration along the jet, and explore different possibilities for the nature of the components within the framework of the bent shocked relativistic jet model.

Modification of exposure conditions by the magnetic field configuration in helicon antenna-excited helium plasma

2020 ◽  
Vol 23 (1) ◽  
pp. 015403
Author(s):  
Tianyuan HUANG ◽  
Peiyu JI ◽  
Jianjun HUANG ◽  
Bin YU ◽  
Xuemei WU
Keyword(s):  
Magnetic Field ◽  
Field Configuration ◽  
Helium Plasma ◽  
Magnetic Field Configuration ◽  
Excited Helium ◽  
The Magnetic Field ◽  
Exposure Conditions

scholarly journals The Two Component Magnetic Field of the Galaxy

1990 ◽  
Vol 140 ◽  
pp. 54-54
Author(s):  
R.R. Andreassian ◽  
A.N. Makarov
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Configuration ◽  
Radio Sources ◽  
Magnetic Field Configuration ◽  
Spiral Arms ◽  
Two Component ◽  
The Galaxy ◽  
The Magnetic Field ◽  
Spiral Arm

The present paper is devoted to a study of the magnetic field configuration of our Galaxy based on Faraday rotation measures (RM) of 185 pulsars and 802 extragalactic radio sources. RM data of pulsars located near the plane of the Galaxy are used for the study of magnetic fields in neighbouring spiral arms. For the distribution of spiral arms the well-known model of Georgelin and Georgelin (1976) is used. The calculations show (for details see Andreassian and Makarov, 1987, 1989) that in the Perseus spiral arm and the local Orion arm the magnetic fields have approximately the same directions (lo;bo) ≈ (80°;0°), while in the Sagittarius-Carina arm the magnetic field has an opposite direction.

FERMION THRESHOLD ENERGY STATES

1992 ◽  
Vol 06 (24) ◽  
pp. 1531-1534
Author(s):  
CHANGHONG ZHU
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Three Dimensional ◽  
Threshold Energy ◽  
Index Theorem ◽  
Equation Of Motion ◽  
Field Configuration ◽  
Two Dimensional ◽  
Magnetic Field Configuration ◽  
The Magnetic Field

We show that for a three-dimensional non-relativistic spinor confined on a plane, the spin-up component obeys the same equation of motion as a two-dimensional spinor. Threshold energy solution is investigated when the electron is moving in the vortex field. It can be proved from the index theorem that the existence of the threshold states depends on the magnetic flux only, not on the magnetic field configuration.

scholarly journals Cosmic ray driven dynamo in barred and ringed galaxies

2010 ◽  
Vol 6 (S274) ◽  
pp. 398-400
Author(s):  
K. Kulpa-Dybeł ◽  
K. Otmianowska-Mazur ◽  
B. Kulesza-Żydzik ◽  
G. Kowal ◽  
D. Wóltański ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Radio Emission ◽  
High Frequency ◽  
Galactic Disk ◽  
Cosmic Ray ◽  
Field Configuration ◽  
Magnetic Field Configuration ◽  
Global Evolution ◽  
Weak Magnetic Fields ◽  
The Magnetic Field

AbstractWe study the global evolution of the magnetic field and interstellar medium (ISM) of the barred and ringed galaxies in the presence of non-axisymmetric components of the potential, i.e. the bar and/or the oval perturbations. The magnetohydrodynamical dynamo is driven by cosmic rays (CR), which are continuously supplied to the disk by supernova (SN) remnants. Additionally, weak, dipolar and randomly oriented magnetic field is injected to the galactic disk during SN explosions. To compare our results directly with the observed properties of galaxies we construct realistic maps of high-frequency polarized radio emission. The main result is that CR driven dynamo can amplify weak magnetic fields up to few μG within few Gyr in barred and ringed galaxies. What is more, the modelled magnetic field configuration resembles maps of the polarized intensity observed in barred and ringed galaxies.

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