Two directional fast imaging of plasma plume in variable magnetic field: Structure and dynamics of the plume in diamagnetic and non-diamagnetic limits

2017 ◽  
Vol 24 (3) ◽  
pp. 033511 ◽  
Author(s):  
Narayan Behera ◽  
R. K. Singh ◽  
V. Chaudhari ◽  
Ajai Kumar
Keyword(s):  
Magnetic Field ◽  
Plasma Plume ◽  
Variable Magnetic Field ◽  
Field Structure ◽  
Fast Imaging ◽  
Magnetic Field Structure ◽  
Structure And Dynamics

The Magnetic-Field Structure and Dynamics of NGC 253

1985 ◽  
pp. 247-248 ◽  
Author(s):  
M. Urbanik ◽  
U. Klein ◽  
R. Beck ◽  
R. Wielebinski
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
Magnetic Field Structure ◽  
Structure And Dynamics ◽  
The Magnetic Field

scholarly journals Image analysis of expanding laser-produced lithium plasma plume in variable transverse magnetic field

2011 ◽  
Vol 29 (2) ◽  
pp. 241-247 ◽  
Author(s):  
Ajai Kumar ◽  
Sony George ◽  
R.K. Singh ◽  
Hem Joshi ◽  
V.P.N. Nampoori
Keyword(s):  
Magnetic Field ◽  
Transverse Magnetic Field ◽  
Plasma Plume ◽  
Imaging Technique ◽  
Transverse Magnetic ◽  
Variable Magnetic Field ◽  
Fast Imaging ◽  
Atomic Processes ◽  
Plasma Parameters ◽  
Lithium Plasma

AbstractUsing fast imaging technique, the effect of transverse magnetic field on the shape and dynamics of the lithium plasma plume has been studied. Enhancement in the overall emission intensity as well as appearance of distinct structures (lobes) in the plasma plume in the presence of magnetic field has been observed. By introducing a variable magnetic field, the influence of J × B force in expanding plasma plume across the transverse magnetic field has been explored. It appears that J × B force does not has a substantial role in the observed structures in the present case rather different atomic processes, which get affected due to change in plasma parameters, are responsible for appearance of these structures.

scholarly journals The magnetic-field structure and dynamics of NGC 253

1985 ◽  
Vol 106 ◽  
pp. 247-248
Author(s):  
M. Urbanik ◽  
U. Klein ◽  
R. Beck ◽  
R. Wielebinski
Keyword(s):  
Magnetic Field ◽  
Radio Telescope ◽  
Field Structure ◽  
Total Power ◽  
Spiral Arms ◽  
Magnetic Field Structure ◽  
Structure And Dynamics ◽  
The Magnetic Field

Total-power and polarization observations of NGC 253 at 10.7 GHz have been performed with the 100-m MPIfR radio telescope. The observed arm/interarm polarization contrasts are discussed in the context of possible field configurations in spiral arms.

scholarly journals The Magnetic Be Star Sigma Orionis E

1987 ◽  
Vol 92 ◽  
pp. 82-83 ◽  
Author(s):  
C. T. Bolton ◽  
A. W. Fullerton ◽  
D. Bohlender ◽  
J. D. Landstreet ◽  
D. R. Gies
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
High Signal ◽  
Rotational Period ◽  
Magnetic Field Structure ◽  
The Past ◽  
Distribution Of Elements ◽  
Be Star ◽  
Hα Emission ◽  
The Magnetic Field

Over the past two years, we have obtained high resolution high signal/noise (S/N) spectra of the magnetic Be star σ Ori E at the Canada-France-Hawaii Telescope and McDonald Observatory. These spectra, which cover the spectral regions 399-417.5 and 440-458.5 nm and the Hα line and have typical S/N>200 and spectral resolution ≃0.02 nm, were obtained at a variety of rotational phases in order to study the magnetic field structure, the distribution of elements in the photosphere, and the effects of the magnetic field on the emission envelope. Our analysis of these spectra confirms, refines and extends the results obtained by Landstreet & Borra (1978), Groote & Hunger (1982 and references therein), and Nakajima (1985).The Hα emission is usually double-peaked, but it undergoes remarkable variations with the 1.19081 d rotational period of the star, which show that the emitting gas is localized into two regions which co-rotate with the star.

scholarly journals Propagation of an MHD Shock in the Vicinity of a Magnetic Neutral Sheet

1980 ◽  
Vol 91 ◽  
pp. 323-326
Author(s):  
D. J. Mullan ◽  
R. S. Steinolfson
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Solar Corona ◽  
Large Scale ◽  
Field Structure ◽  
Neutral Sheet ◽  
Solar Cosmic Rays ◽  
Magnetic Field Structure ◽  
Large Scale Magnetic Field ◽  
Highly Correlated

The acceleration of solar cosmic rays in association with certain solar flares is known to be highly correlated with the propagation of an MHD shock through the solar corona (Svestka, 1976). The spatial structure of the sources of solar cosmic rays will be determined by those regions of the corona which are accessible to the flare-induced shock. The regions to which the flare shock is permitted to propagate are determined by the large scale magnetic field structure in the corona. McIntosh (1972, 1979) has demonstrated that quiescent filaments form a single continuous feature (a “baseball stitch”) around the surface of the sun. It is known that helmet streamers overlie quiescent filaments (Pneuman, 1975), and these helmet streamers contain large magnetic neutral sheets which are oriented essentially radially. Hence the magnetic field structure in the low solar corona is characterized by a large-scale radial neutral sheet which weaves around the entire sun following the “baseball stitch”. There is therefore a high probability that as a shock propagates away from a flare, it will eventually encounter this large neutral sheet.

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