scholarly journals CONDUCTOMETRIC EVALUATION OF ASSOCIATION CONSTANTS FOR AQUEOUS SOLUTIONS OF CoCl2 IN THE ABSENCE AND PRESENCE OF A MAGNETIC FIELD

2009 ◽  
Vol 17 (17) ◽  
pp. 33-40
Author(s):  
Maany A. Hamada ◽  
Nagah El-Shishtawi ◽  
Esam A. Gomaa
Keyword(s):  
Magnetic Field ◽  
Aqueous Solutions ◽  
Average Power ◽  
Association Constants ◽  
Experimental Conductivity ◽  
New Equation ◽  
The Magnetic Field

The association constants KA for CoCl2 aqueous solutions were calculated using the experimental conductivity values at different salt concentrations. The molar conductivities were measured in the absence and presence of a magnetic field with an average power of 0. 677 KGauss. A new equation for asymmetric 1:2 salts was suggested and used. This equation was derived from Ostwald, Arrhenius, and Fuoss-Shedlovsky theories. The results obtained were discussed and the effect of the magnetic field on the association constants was explained.

scholarly journals The Effect of Magnetic Field Strength and Geometry on the Deposition Rate and Ionized Flux Fraction in the HiPIMS Discharge

Plasma ◽  
2019 ◽  
Vol 2 (2) ◽  
pp. 201-221 ◽  
Author(s):  
Hamidreza Hajihoseini ◽  
Martin Čada ◽  
Zdenek Hubička ◽  
Selen Ünaldi ◽  
Michael A. Raadu ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Deposition Rate ◽  
Average Power ◽  
Current Mode ◽  
Ionization Probability ◽  
Cathode Voltage ◽  
Peak Current ◽  
Voltage Mode ◽  
Operating Modes ◽  
The Magnetic Field

We explored the effect of magnetic field strength | B | and geometry (degree of balancing) on the deposition rate and ionized flux fraction F flux in dc magnetron sputtering (dcMS) and high power impulse magnetron sputtering (HiPIMS) when depositing titanium. The HiPIMS discharge was run in two different operating modes. The first one we refer to as “fixed voltage mode” where the cathode voltage was kept fixed at 625 V while the pulse repetition frequency was varied to achieve the desired time average power (300 W). The second mode we refer to as “fixed peak current mode” and was carried out by adjusting the cathode voltage to maintain a fixed peak discharge current and by varying the frequency to achieve the same average power. Our results show that the dcMS deposition rate was weakly sensitive to variations in the magnetic field while the deposition rate during HiPIMS operated in fixed voltage mode changed from 30% to 90% of the dcMS deposition rate as | B | decreased. In contrast, when operating the HiPIMS discharge in fixed peak current mode, the deposition rate increased only slightly with decreasing | B | . In fixed voltage mode, for weaker | B | , the higher was the deposition rate, the lower was the F flux . In the fixed peak current mode, both deposition rate and F flux increased with decreasing | B | . Deposition rate uniformity measurements illustrated that the dcMS deposition uniformity was rather insensitive to changes in | B | while both HiPIMS operating modes were highly sensitive. The HiPIMS deposition rate uniformity could be 10% lower or up to 10% higher than the dcMS deposition rate uniformity depending on | B | and in particular the magnetic field topology. We related the measured quantities, the deposition rate and ionized flux fraction, to the ionization probability α t and the back attraction probability of the sputtered species β t . We showed that the fraction of the ions of the sputtered material that escape back attraction increased by 30% when | B | was reduced during operation in fixed peak current mode while the ionization probability of the sputtered species increased with increasing | B | , due to increased discharge current, when operating in fixed voltage mode.

The magnetic field dependence of water proton T 1 in aqueous solutions: Implications for magnetic imaging contrast media

1984 ◽  
Vol 11 (5) ◽  
pp. 712-713 ◽  
Author(s):  
Robert G. Bryant ◽  
Carl Polnaszek ◽  
Scott Kennedy ◽  
Joanne Hetzler ◽  
David Hickerson
Keyword(s):  
Magnetic Field ◽  
Contrast Media ◽  
Aqueous Solutions ◽  
Field Dependence ◽  
Magnetic Field Dependence ◽  
Water Proton ◽  
Magnetic Imaging ◽  
The Magnetic Field

scholarly journals Светорассеяние в воде и водных растворах, находящихся под действием слабого магнитного поля

2019 ◽  
Vol 126 (6) ◽  
pp. 713
Author(s):  
Л.А. Булавин ◽  
Л.Ю. Вэргун ◽  
Ю.Ф. Забашта ◽  
О.С. Свечникова ◽  
Е.О. Огородник
Keyword(s):  
Magnetic Field ◽  
Aqueous Solution ◽  
Light Scattering ◽  
Aqueous Solutions ◽  
Glucose Solution ◽  
Scattering Intensity ◽  
Large Fluctuations ◽  
The Magnetic Field

AbstractLight scattering in water and aqueous solutions of NaCl and glucose under the action of a magnetic field with an induction of 0.43 mT is studied. It is established that the magnetic field does not affect the light scattering in water and aqueous solution of NaCl. For an aqueous glucose solution, the switching on of a field leads to the appearance of large fluctuations in the scattering intensity. It has been shown that these fluctuations are due to turbulization of the solution that is caused by the magnetic field.

scholarly journals Equation of State of Strongly Magnetized Matter with Hyperons and Δ-Resonances

Particles ◽  
2020 ◽  
Vol 3 (4) ◽  
pp. 660-675 ◽  
Author(s):  
Vivek Baruah Thapa ◽  
Monika Sinha ◽  
Jia Jie Li ◽  
Armen Sedrakian
Keyword(s):  
Magnetic Field ◽  
Equation Of State ◽  
Density Functional ◽  
Oscillatory Behavior ◽  
Functional Theory ◽  
Intense Magnetic Field ◽  
New Equation ◽  
Covariant Density ◽  
The Magnetic Field ◽  
Magnetic Case

We construct a new equation of state for the baryonic matter under an intense magnetic field within the framework of covariant density functional theory. The composition of matter includes hyperons as well as Δ-resonances. The extension of the nucleonic functional to the hypernuclear sector is constrained by the experimental data on Λ and Ξ-hypernuclei. We find that the equation of state stiffens with the inclusion of the magnetic field, which increases the maximum mass of neutron star compared to the non-magnetic case. In addition, the strangeness fraction in the matter is enhanced. Several observables, like the Dirac effective mass, particle abundances, etc. show typical oscillatory behavior as a function of the magnetic field and/or density which is traced back to the occupation pattern of Landau levels.

scholarly journals Reevaluation and correction of Maxwell’s Equations: a magnetic field has a source, a moving electric charge

F1000Research ◽  
2020 ◽  
Vol 9 ◽  
pp. 1092
Author(s):  
M.J. Koziol
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Electric Charge ◽  
Maxwell’S Equations ◽  
Maxwell's Equations ◽  
Electric And Magnetic Fields ◽  
The World ◽  
New Equation ◽  
The Magnetic Field

Maxwell’s Equations are considered to summarize the world of electromagnetism in four elegant equations. They summarize how electric and magnetic fields propagate, interact, how they are influenced by other objects and what their sources are. While it is widely accepted that the source of a magnetic field is a moving charge, one of the equations instead states that the magnetic field has no source. However, it is widely accepted that a magnetic field cannot be created without a moving electric charge. As such, here, after carefully reevaluating how Maxwell derived his equation, a limitation was identified. After adjustments, a new equation was derived that instead demonstrates that the source of a magnetic field is a moving charge, confirming experimentally verified and widely accepted observations.

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.

Evolution of Large-Scale Coronal Structures

1994 ◽  
Vol 144 ◽  
pp. 29-33
Author(s):  
P. Ambrož
Keyword(s):  
Magnetic Field ◽  
Field Line ◽  
Large Scale ◽  
Coronal Magnetic Field ◽  
Source Surface ◽  
Solar Cycles ◽  
Characteristic Relationship ◽  
The Magnetic Field ◽  
Coronal Structures

AbstractThe large-scale coronal structures observed during the sporadically visible solar eclipses were compared with the numerically extrapolated field-line structures of coronal magnetic field. A characteristic relationship between the observed structures of coronal plasma and the magnetic field line configurations was determined. The long-term evolution of large scale coronal structures inferred from photospheric magnetic observations in the course of 11- and 22-year solar cycles is described.Some known parameters, such as the source surface radius, or coronal rotation rate are discussed and actually interpreted. A relation between the large-scale photospheric magnetic field evolution and the coronal structure rearrangement is demonstrated.

Emergence of Twisted Magnetic Flux Related Sigmoidal Brightening

2000 ◽  
Vol 179 ◽  
pp. 263-264
Author(s):  
K. Sundara Raman ◽  
K. B. Ramesh ◽  
R. Selvendran ◽  
P. S. M. Aleem ◽  
K. M. Hiremath
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Ultra Violet ◽  
Active Regions ◽  
Morphological Properties ◽  
Energy Storage And Conversion ◽  
The Sun ◽  
X Rays ◽  
The Magnetic Field

Extended AbstractWe have examined the morphological properties of a sigmoid associated with an SXR (soft X-ray) flare. The sigmoid is cospatial with the EUV (extreme ultra violet) images and in the optical part lies along an S-shaped Hαfilament. The photoheliogram shows flux emergence within an existingδtype sunspot which has caused the rotation of the umbrae giving rise to the sigmoidal brightening.It is now widely accepted that flares derive their energy from the magnetic fields of the active regions and coronal levels are considered to be the flare sites. But still a satisfactory understanding of the flare processes has not been achieved because of the difficulties encountered to predict and estimate the probability of flare eruptions. The convection flows and vortices below the photosphere transport and concentrate magnetic field, which subsequently appear as active regions in the photosphere (Rust & Kumar 1994 and the references therein). Successive emergence of magnetic flux, twist the field, creating flare productive magnetic shear and has been studied by many authors (Sundara Ramanet al.1998 and the references therein). Hence, it is considered that the flare is powered by the energy stored in the twisted magnetic flux tubes (Kurokawa 1996 and the references therein). Rust & Kumar (1996) named the S-shaped bright coronal loops that appear in soft X-rays as ‘Sigmoids’ and concluded that this S-shaped distortion is due to the twist developed in the magnetic field lines. These transient sigmoidal features tell a great deal about unstable coronal magnetic fields, as these regions are more likely to be eruptive (Canfieldet al.1999). As the magnetic fields of the active regions are deep rooted in the Sun, the twist developed in the subphotospheric flux tube penetrates the photosphere and extends in to the corona. Thus, it is essentially favourable for the subphotospheric twist to unwind the twist and transmit it through the photosphere to the corona. Therefore, it becomes essential to make complete observational descriptions of a flare from the magnetic field changes that are taking place in different atmospheric levels of the Sun, to pin down the energy storage and conversion process that trigger the flare phenomena.

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