To: “Magnetic Anomaly Due to a Vertical Right Circular Cylinder with Arbitrary Polarization”, by S. K. Singh and F. J. Sabina, GEOPHYSICS, v. 43, p. 173–178 (February, 1978)

Geophysics ◽  
1978 ◽  
Vol 43 (6) ◽  
pp. 1312-1312
Keyword(s):  
Magnetic Field ◽  
Circular Cylinder ◽  
Magnetic Anomaly ◽  
Arbitrary Polarization ◽  
Right Hand ◽  
The Right ◽  
The Magnetic Field

There is an error in the paper “Magnetic Anomaly Due to a Vertical Right Circular Cylinder with Arbitrary Polarization”, by S. K. Singh and F. J. Sabina, Geophysics, v. 43, p. 173–178 (February, 1978). The second term of the right‐hand side of equation (5) should be negative. The equation should read: [Formula: see text]. The plot of the magnetic field in Figures 2–4 is correct.

MAGNETIC ANOMALY DUE TO A VERTICAL RIGHT CIRCULAR CYLINDER WITH ARBITRARY POLARIZATION

Geophysics ◽  
1978 ◽  
Vol 43 (1) ◽  
pp. 173-178 ◽  
Author(s):  
Shri Krishna Singh ◽  
Federico J. Sabina
Keyword(s):  
Magnetic Field ◽  
Circular Cylinder ◽  
Closed Form ◽  
Magnetic Anomaly ◽  
Closed Form Solution ◽  
Form Solution ◽  
Arbitrary Polarization ◽  
Shaped Body ◽  
Anomalous Magnetic Field

A closed form solution for the total anomalous magnetic field due to a vertical right circular cylinder with arbitrary polarization is derived under the assumption that the magnetization is uniform. As expected, the computed field is similar to the field due to a “similar” prism‐shaped body.

scholarly journals Alfvén Waves in Dusty Interstellar Clouds

1997 ◽  
Vol 14 (2) ◽  
pp. 170-178 ◽  
Author(s):  
N. F. Cramer ◽  
S. V. Vladimirov
Keyword(s):  
Magnetic Field ◽  
Negative Charge ◽  
Alfven Waves ◽  
Dust Particles ◽  
Alfvén Waves ◽  
Interstellar Clouds ◽  
General Dispersion ◽  
The Right ◽  
The Magnetic Field ◽  
Field Wave

AbstractDust particles in a plasma can be higWy charged, and can carry a proportion of the negative charge of the plasma. Even if this proportion is quite small, as in interstellar dusty clouds, it can have a large effect on hydromagnetic Alfvén waves propagating at frequencies well below the ion–cyclotron frequency. In particular, the right-hand circularly polarised mode experiences a cutoff due to the presence of the dust. We generalise previous work on Alfvén waves in dusty interstellar plasmas by considering the general dispersion relation for waves propagating at an arbitrary angle with respect to the magnetic field. Wave energy propagating at oblique angles to the magnetic field in an increasing density gradient can be very efficiently damped by the Alfvén resonance absorption process in a dusty plasma, and we consider this damping mechanism for waves in interstellar clouds.

Swirling Flow of Magnetic Fluid in Multi-Pole Rotating Magnetic Field

2003 ◽  
Author(s):  
Kenichi Kamioka ◽  
Ryuichiro Yamane
Keyword(s):  
Magnetic Field ◽  
Fluid Flow ◽  
Circular Cylinder ◽  
Phase Velocity ◽  
Magnetic Fluid ◽  
Swirling Flow ◽  
Peak Velocity ◽  
Rotating Magnetic Field ◽  
Outer Periphery ◽  
The Magnetic Field

The experiments are conducted on the magnetic fluid flow induced by the multi-pole rotating magnetic field in a circular cylinder. The numbers of poles are two, four, six, eight and twelve. The applied electric current and frequency are 2∼6 A and 20∼60 Hz, respectively. The peak velocity of the flow increases with the increase in the strength and the phase velocity of the magnetic field. As the increase in the number of poles, the flow shifts to the outer periphery.

The distortion of a magnetic field by the flow of a conducting fluid past a circular cylinder

1965 ◽  
Vol 22 (3) ◽  
pp. 561-578 ◽  
Author(s):  
R. Seebass ◽  
K. Tamada
Keyword(s):  
Magnetic Field ◽  
Integral Equation ◽  
Circular Cylinder ◽  
Potential Flow ◽  
Uniform Magnetic Field ◽  
The Body ◽  
Flow Potential ◽  
Field Lines ◽  
The Magnetic Field ◽  
Rear Stagnation Point

The distortion of a uniform magnetic field, aligned with the flow at infinity, by the potential flow of an inviscid conductor about a circular cylinder is determined. Potential flow of the fluid occurs when the interaction parameter is small; this is the case studied here. In the flow-potential and stream-function plane the problem may be formulated as a singular integral equation. Solutions of this equation show that for small fluid conductivities the magnetic field lines are distorted in the sense of being dragged along by the motion of the fluid. This process continues as the conductivity increases, with fewer and fewer of the magnetic field lines entering the body. For large conductivity this reduced flux of field lines enters over most of the body surface and exits in the neighbourhood of the rear stagnation point; behind the body there is a jet-like structure of magnetic field lines.

Dynamics of a Partially Full Cylinder Containing a Magnetic Liquid in a Magnetic Field

1976 ◽  
Vol 43 (3) ◽  
pp. 497-501
Author(s):  
D. R. Tichenor ◽  
X. J. R. Avula
Keyword(s):  
Magnetic Field ◽  
Free Surface ◽  
Circular Cylinder ◽  
Plane Surface ◽  
Equations Of Motion ◽  
Magnetic Liquid ◽  
Transient Motion ◽  
Thin Walled ◽  
Inclined Planes ◽  
The Magnetic Field

This study is concerned with the transient motion of an infinitely long thin-walled circular cylinder partially filled with a magnetic liquid under magnetic and nonmagnetic forces. Starting from rest the cylinder is constrained to roll without slipping on a plane surface while the contained fluid with a rectangular free surface is simultaneously subjected to a magnetic field parallel to the plane by activating a magnet located ahead of the cylinder. The nonmagnetic force on the cylinder and its contents is provided by the gravity. Assuming negligible viscous dissipation Lagrange’s equations of motion are derived and solved to obtain the motion of the cylinder and the liquid subsequent to the application of the magnetic field. Results are presented in a nondimensional form for motion on horizontal and inclined planes under different magnetic strengths.

A Dynamo Model for Magnetic Stars with Long Periods

1976 ◽  
Vol 32 ◽  
pp. 39-42
Author(s):  
M. Schüssler
Keyword(s):  
Magnetic Field ◽  
Main Sequence ◽  
Convection Zone ◽  
Dynamo Model ◽  
Magnetic Stars ◽  
Order Of Magnitude ◽  
Linear Effects ◽  
The Right ◽  
Right Order ◽  
The Magnetic Field

SummaryA α - effect dynamo model is presented which can be relevant for the group of magnetic stars.with observed periods between 1 y and 72 ys. The model is based on an axisymmetric α2- dynamo including non-linear effects due to the “cut off α- effect”; no differential rotation is taken into account. There are oscilliations of the magnetic field with periods in the right order of magnitude under the assumption of an outer convection zone between R ≥ r ≥.5 R ….7R. In the sense of this model therefore these stars should be young objects passing from their Hayashi track down to the main sequence.

VISCOELASTIC FLUID FLOW PASS A POROUS CIRCULAR CYLINDER WHEN THE MAGNETIC FIELD INCLUDED

2015 ◽  
Vol 99 (2) ◽  
pp. 173-186 ◽  
Author(s):  
Basuki Widodo ◽  
Chairul Imron ◽  
Nur Asiyah ◽  
Galuh Oktavia Siswono ◽  
Tri Rahayuningsih ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Fluid Flow ◽  
Circular Cylinder ◽  
Viscoelastic Fluid ◽  
The Magnetic Field

The Position of a Type I Storm Source in the Magnetic Field of an Active Region

1973 ◽  
Vol 2 (4) ◽  
pp. 211-214 ◽  
Author(s):  
G. A. Dulk ◽  
G. J. Nelson
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Type I ◽  
Bipolar Structure ◽  
Circularly Polarized ◽  
One Dimensional ◽  
Left Hand ◽  
Right Hand ◽  
Sun Spots ◽  
The Magnetic Field

Type I storms generally occur in association with large sun-spots and the radiation is usually circularly polarized. Statistically it has been found that the sense of polarization, right-hand (RH) or left-hand (LH), usually corresponds to the ordinary magneto-ionic mode in the field of the dominant spot of the active region; when a following spot dominates, the polarization tends to be determined by this spot rather than by the leading field. One-dimensional position measurements show that the type I sources are usually not radially above the active region but are displaced by a few minutes of arc. The source sizes are about l′.2 to 4′.5 at 169 MHz and the sources frequently contain double, multiple or bipolar structure at 80 and 160 MHz.

The search for electromagnetic induction, 1820-1831

1965 ◽  
Vol 20 (2) ◽  
pp. 184-219 ◽  
Keyword(s):  
Magnetic Field ◽  
Electromagnetic Induction ◽  
The United States ◽  
Single Wire ◽  
Electricity And Magnetism ◽  
Magnetic Meridian ◽  
The Right ◽  
The University ◽  
The Magnetic Field ◽  
Do So

Oersted´s discovery in 1820 of the magnetic field that surrounds a conductor during the passage of an electric current, aroused a wave of interest among men of science in England, France, Germany, Italy, and the United States. The apparatus required to verify his results was easily put together, and anyone who cared to do so could see for himself the nature of the indissoluble connexion between electricity and magnetism, which, though long suspected and vaguely adumbrated, was now precisely defined and made a permanent portion of the corpus of science. As one subsequent discovery after another was announced from various places, the recognition became widespread that a large and unexploited field for investigations and applications had been opened up. Only one week after word of Oersted’s experiment reached Paris, Ampere discovered that two parallel wires that carry parallel currents attract each other. Less than two months after Oersted’s publication, J. S. C. Schweigger (1779-1857), at the University of Halle, reasoned that if the current in a single wire held above the compass needle would deflect the needle to the right, while the same wire placed beneath the needle would deflect it to the left, one turn of wire, placed around the needle in the plane of the magnetic meridian, would exert twice the deflecting force of a single wire; and a coil made of ten turns of insulated wire would exert twenty times the force.

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