On the diffusion and clustering of a magnetic field in random velocity fields

2009 ◽  
Vol 109 (2) ◽  
pp. 345-356 ◽  
Author(s):  
V. I. Klyatskin ◽  
O. G. Chkhetiani
Keyword(s):  
Magnetic Field ◽  
Velocity Fields ◽  
Random Velocity

A Discussion on solar studies with special reference to space observations - The manifold structure of the chromosphere and corona

1971 ◽  
Vol 270 (1202) ◽  
pp. 77-80 ◽  
Keyword(s):  
Magnetic Field ◽  
Fine Structure ◽  
High Resolution ◽  
Field Strength ◽  
Special Reference ◽  
Velocity Fields ◽  
Field Patterns ◽  
Uniform Region ◽  
Determining Factor ◽  
The Magnetic Field

Although the photosphere is a uniform region for scales greater than the granulation, the fact that the magnetic field strength falls off less sharply than the gas pressure leads to strong magnetic influence at greater heights in the solar atmosphere. This magnetic influence leads to non-uniformity and fine structure in the chromosphere and corona. The existence of such structure has been deduced mostly from measurements of photospheric phenomena; in particular, from measurements of photospheric velocity fields (Leighton, Noyes & Simon 1962) and of photospheric magnetic fields (Bumba & Howard 1965). The determining factor would thus appear to be in the photosphere; but visible effects only are produced in the chromosphere and corona. In recent years, high resolution filter photography has enabled us to recognize different regions of the chromosphere, where qualitatively different structure is associated with distinct magnetic field patterns. This progress has been possible because of better Lyot filters, better films and better observing sites; the spectroheliograph has always been limited for high resolution work by the finite slit width and the difficulty of accurate guiding during the long exposures.

A Discussion on the physics of the solar atmosphere - Physics of the solar atmosphere

1976 ◽  
Vol 281 (1304) ◽  
pp. 415-426
Keyword(s):  
Magnetic Field ◽  
Transition Region ◽  
Solar Atmosphere ◽  
Solar Rotation ◽  
Active Regions ◽  
Rotation Velocity ◽  
Coronal Magnetic Field ◽  
Velocity Fields ◽  
Field Structure ◽  
Magnetic Field Structure

A summary is given on recent results on the physics of the quiet solar atmosphere, and active regions. This includes: solar rotation, velocity fields and waves, magnetic field concentration, the transition region, coronal magnetic field structure, and prominences.

scholarly journals Progress in the Measurement of Solar Magnetic Fields

1993 ◽  
Vol 141 ◽  
pp. 149-155 ◽  
Author(s):  
Guoxiang Ai
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
White Light ◽  
Historical Development ◽  
Solar Magnetic Field ◽  
Solar Physics ◽  
Monochromatic Light ◽  
Velocity Fields ◽  
Solar Magnetic Fields ◽  
Optical Instruments

AbstractThe historical development of optical instruments for solar physics is outlined, from white light to unpolarized and polarized monochromatic light, to Stokes profiles and simultaneous fields of view, from points to lines, plane to cube. An evolutionary series and classificaton of instruments for the solar magnetic field is described. As a next step the 2-D real time polarizing spectrograph has been proposed. The planned instruments in China for measurements of solar magnetic and velocity fields are briefly introduced.

scholarly journals Unsteady Flow and Heat Transfer of a Dusty Fluid through a Rectangular Channel

2010 ◽  
Vol 2010 ◽  
pp. 1-17 ◽  
Author(s):  
B. J. Gireesha ◽  
G. S. Roopa ◽  
C. S. Bagewadi
Keyword(s):  
Magnetic Field ◽  
Heat Transfer ◽  
Unsteady Flow ◽  
Uniform Magnetic Field ◽  
Rectangular Channel ◽  
Velocity Fields ◽  
Dusty Fluid ◽  
Flow And Heat Transfer ◽  
Pulsatile Pressure ◽  
Pulsatile Pressure Gradient

The present discussion deals with the study of an unsteady flow and heat transfer of a dusty fluid through a rectangular channel under the influence of pulsatile pressure gradient along with the effect of a uniform magnetic field. The analytical solutions of the problem are obtained using variable separable and Fourier transform techniques. The graphs are drawn for the velocity fields of both fluid and dust phases under the effect of Reynolds number. Further, changes in the Nusselt number are shown graphically, and, on the basis of these, the conclusions and discussions are given.

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