scholarly journals Dynamic Behaviour of Oscillating Bubbles inside a Nonlinear Thixotropic Fluid in Existence of Magnetic Field

2019 ◽  
Author(s):  
Alireza Taklifi
Keyword(s):  
Magnetic Field ◽  
Dynamic Behaviour ◽  
Oscillating Bubbles ◽  
Thixotropic Fluid

Dynamik des Zerfalls von Inversionswänden in einem nematischen flüssigen Kristall / Dynamics of the Annihilation of Inversion Walls in a Nernatic Liquid Crystal

1974 ◽  
Vol 29 (9) ◽  
pp. 1356-1366 ◽  
Author(s):  
G. Heppke ◽  
F. Schneider
Keyword(s):  
Magnetic Field ◽  
Liquid Crystal ◽  
Electric Conductivity ◽  
Dynamic Behaviour ◽  
Numerical Procedure ◽  
Experimental Results ◽  
Conductivity Measurements

Inversion walls are generated by rotating the direction of a magnetic field by 180° with respect to the director in the homeotropically aligned nematic layer. A numerical procedure based on the Leslie-Ericksen theory allows for the calculation of the dynamic behaviour of the inversion walls. Experimental results obtained with MBBA by electric conductivity measurements show satisfying agreement with theory.

Theoretical Foucault Images of Superconducting Fluxons

1997 ◽  
Vol 3 (S2) ◽  
pp. 509-510
Author(s):  
M. Beleggia ◽  
G. Pozzi ◽  
K. Harada ◽  
H. Kasai ◽  
T. Matsuda ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Dynamic Behaviour ◽  
Structural Defects ◽  
Experimental Conditions ◽  
Transmitted Beam ◽  
Factors Affecting ◽  
One Dimensional ◽  
Flux Lines ◽  
Main Disadvantage ◽  
Individual Flux

Individual flux lines in superconducting specimens have been recently observed using a 300kV holography electron microscope equipped with a cold field emission gun in the transmission mode by means of the out-of-focus method. In this way it has been possible to observe the dynamic behaviour of fluxons depending upon the variations of the temperature and/or the applied magnetic field or current. The main disadvantage of this method is that correlation with structural defects is troublesome owing to the large defocus distance (of the order of 1 cm for conventional superconductors) necessary for the detection of flux lines.This drawback is not present in the Foucault technique, where the contrast is generated in the focused image by masking part of the transmitted beam by means of an aperture. Therefore, some preliminary calculations have been made recently using one-dimensional models, which allow for a quick and easy simulation of the factors affecting the experimental conditions .

The dynamic behaviour of magnetic levitating magnet-magnetic fluid element in alternating magnetic field

2012 ◽  
Vol 39 (1-4) ◽  
pp. 595-601
Author(s):  
Seiichi Sudo ◽  
Takumi Goto ◽  
Michihiro Shinozaki ◽  
Toshiya Kainuma ◽  
Hidemasa Takana ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fluid ◽  
Dynamic Behaviour ◽  
Alternating Magnetic Field ◽  
Fluid Element

Influence of magnetic field on laser-produced barium plasmas: Spectral and dynamic behaviour of neutral and ionic species

2014 ◽  
Vol 116 (15) ◽  
pp. 153301 ◽  
Author(s):  
Makaraju Srinivasa Raju ◽  
R. K. Singh ◽  
Pramod Gopinath ◽  
Ajai Kumar
Keyword(s):  
Magnetic Field ◽  
Dynamic Behaviour ◽  
Ionic Species

scholarly journals Physical Analysis of Low-dynamic Magnetic Field Impact on Human Tissue

2020 ◽  
Vol 7 (1) ◽  
pp. 14-17 ◽  
Author(s):  
Aleš Richter ◽  
Želmíra Ferková ◽  
Václav Bittner
Keyword(s):  
Magnetic Field ◽  
Muscle Tissue ◽  
Human Body ◽  
Human Tissue ◽  
Electromagnetic Induction ◽  
Dynamic Behaviour ◽  
Physical Analysis ◽  
Power Sources ◽  
Metal Implants ◽  
Dynamic Magnetic Field

This article makes an effort to explain physical aspects of low-dynamic magnetic field in the human tissue. The principles of electromagnetic induction in the muscle tissue as a typical example of parts of human body are briefly presented. The problems are indicated by modelling. One of the goals is to warn about different distribution of magnetic field in parts of body caused by metal implants. Another analyse introduces physical and energy differences among individual types of power sources of magnetic field and their dynamic behaviour.

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

Structure in the radiation of the galactic disk

1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Galactic Disk ◽  
Galactic Magnetic Field ◽  
Measured Polarization

Observations at various frequencies between 136 and 1400 MHz indicate a considerable amount of structure in the galactic disk. This result appears consistent both with measured polarization percentages and with considerations of the strength of the galactic magnetic field.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

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