The flow of conducting fluids through circular pipes having finite conductivity and finite thickness under uniform transverse magnetic fields

1981 ◽  
Vol 19 (9) ◽  
pp. 1221-1232 ◽  
Author(s):  
SK.Abdus Samad
Keyword(s):  
Magnetic Fields ◽  
Finite Thickness ◽  
Transverse Magnetic ◽  
Finite Conductivity ◽  
Circular Pipes ◽  
Conducting Fluids

The Flow of Conducting Fluids in Circular Pipes With Finite Conductivity Under Uniform Transverse Magnetic Fields

1967 ◽  
Vol 34 (1) ◽  
pp. 29-36 ◽  
Author(s):  
Sadatoshi Ihara ◽  
Kiyohiro Tajima ◽  
Akira Matsushima
Keyword(s):  
Theoretical Calculations ◽  
Transverse Magnetic ◽  
Skin Friction Coefficient ◽  
Finite Conductivity ◽  
Electrically Conducting ◽  
Wall Conductivity ◽  
Circular Pipes ◽  
Poiseuille Number ◽  
Conducting Fluids ◽  
Good Agreement

The flow of incompressible, viscous, electrically conducting fluids in circular pipes in the presence of an applied transverse magnetic field is analyzed theoretically and experimentally. The relations among the Hartmann number, the Poiseuille number, skin friction coefficient, the Reynolds number, sensitivity, and wall conductivity are discussed. The experimental results using carbon pipe, stainless-steel pipe, and glass pipe are in good agreement with theoretical calculations.

Steady motion of conducting fluids in pipes under transverse magnetic fields

1953 ◽  
Vol 49 (1) ◽  
pp. 136-144 ◽  
Author(s):  
J. A. Shercliff
Keyword(s):  
Velocity Profile ◽  
Rectangular Channel ◽  
Steady Motion ◽  
Transverse Magnetic ◽  
Pressure Gradients ◽  
Electrically Conducting ◽  
Degenerate Solution ◽  
Circular Pipes ◽  
Induced Currents ◽  
Conducting Fluids

ABSTRACTThis paper studies the steady motion of an electrically conducting, viscous fluid along channels in the presence of an imposed transverse magnetic field when the walls do not conduct currents. The equations which determine the velocity profile, induced currents and field are derived and solved exactly in the case of a rectangular channel. When the imposed field is sufficiently strong the velocity profile is found to degenerate into a core of uniform flow surrounded by boundary layers on each wall. The layers on the walls parallel to the imposed field are of a novel character. An analogous degenerate solution for channels of any symmetrical shape is developed. The predicted pressure gradients for given volumes of flow at various field strengths are finally compared with experimental results for square and circular pipes.

Radio Measurements of Coronal Magnetic Fields

1994 ◽  
Vol 144 ◽  
pp. 21-28 ◽  
Author(s):  
G. B. Gelfreikh
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Active Regions ◽  
High Sensitivity ◽  
Coronal Magnetic Field ◽  
Transverse Magnetic ◽  
Radio Sources ◽  
Radio Waves ◽  
Solar Active Regions

AbstractA review of methods of measuring magnetic fields in the solar corona using spectral-polarization observations at microwaves with high spatial resolution is presented. The methods are based on the theory of thermal bremsstrahlung, thermal cyclotron emission, propagation of radio waves in quasi-transverse magnetic field and Faraday rotation of the plane of polarization. The most explicit program of measurements of magnetic fields in the atmosphere of solar active regions has been carried out using radio observations performed on the large reflector radio telescope of the Russian Academy of Sciences — RATAN-600. This proved possible due to good wavelength coverage, multichannel spectrographs observations and high sensitivity to polarization of the instrument. Besides direct measurements of the strength of the magnetic fields in some cases the peculiar parameters of radio sources, such as very steep spectra and high brightness temperatures provide some information on a very complicated local structure of the coronal magnetic field. Of special interest are the results found from combined RATAN-600 and large antennas of aperture synthesis (VLA and WSRT), the latter giving more detailed information on twodimensional structure of radio sources. The bulk of the data obtained allows us to investigate themagnetospheresof the solar active regions as the space in the solar corona where the structures and physical processes are controlled both by the photospheric/underphotospheric currents and surrounding “quiet” corona.

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