The Effect of Magnetic Field on The Solubility of NaCl and CaCl2.2H2O at Different Temperature and pH Values

2012 ◽  
Vol 25 (1) ◽  
pp. 19-26 ◽  
Author(s):  
Tariq N. Musa
Keyword(s):  
Magnetic Field ◽  
Ph Values

Synergy Remediation of PBDEs Contaminated Soil by Electric-Magnetic Method

2013 ◽  
Vol 726-731 ◽  
pp. 2338-2341 ◽  
Author(s):  
Chun Du Wu ◽  
Yi Fan Yao ◽  
Qing Jie Xie
Keyword(s):  
Magnetic Field ◽  
Contaminated Soil ◽  
Polybrominated Diphenyl Ethers ◽  
Uniform Magnetic Field ◽  
Uniform Electric Field ◽  
Magnetic Method ◽  
Acid Base ◽  
Ph Values ◽  
Diphenyl Ethers ◽  
Soil Area

An electrokinetic and magnetic remediation system of polybrominated diphenyl ethers (PBDEs) contaminated soil was built in the laboratory. The characteristics of BDE15 migration under non-uniform electric field and uniform magnetic field were investigated. The results indicated that current and temperature in the soil reached the maximum values 100mA and 14°C respectively in 6h; the moisture content of soil near the cathode and anode was higher than in the middle position; pH values of soil increased gradually from the anode to the cathode and acid-base interface was in the soil area between 3cm from anode and 5 cm from anode; BDE15 mainly enriched in the area 5cm from the anode and reached 22.69μg·g-1.

scholarly journals On Nature of the Induced Anisotropy in the Chemically Deposited Со‒Р Films

2018 ◽  
Vol 185 ◽  
pp. 03012 ◽  
Author(s):  
Anatoly V. Chzhan ◽  
Sergey A. Podorozhnyak ◽  
Mikhail N. Volochaev ◽  
Gennady S. Patrin
Keyword(s):  
Magnetic Field ◽  
Magnetic Anisotropy ◽  
Relaxation Times ◽  
Chemical Deposition ◽  
Induced Anisotropy ◽  
Pronounced Difference ◽  
Physical Mechanisms ◽  
Ph Values ◽  
Induced Magnetic Anisotropy ◽  
Liquid Solutions

The induced magnetic anisotropy in the Со‒Рfilms prepared by chemical deposition from liquid solutions in a magnetic field has been investigated. The pronounced difference between the anisotropy values and relaxation times points out the existence of different physical mechanisms responsible for the occurrence of anisotropy of the Со‒Р films at low and high pH values. Possible mechanisms of the induced anisotropy in the Со‒Р films prepared at different pH values are discussed.

scholarly journals In vitro and in vivo comparison of the MRI glucoCEST properties between native glucose and 3OMG in a murine tumor model

2021 ◽  
Author(s):  
Annasofia Anemone ◽  
Martina Capozza ◽  
Francesca Arena ◽  
Sara Zullino ◽  
Paola Bardini ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Ph Dependence ◽  
Power Level ◽  
Tumor Model ◽  
Murine Models ◽  
Ph Values ◽  
Saturation Power ◽  
Glucose Derivatives

ABSTRACTPurposeD-Glucose and 3-O-Methyl-D-glucose (3OMG) have been shown to provide contrast in MRI-CEST images. However, a systematic comparison between these two molecules has not yet been performed. This study dealt with the assessment of the effect of pH, saturation power level (B1) and magnetic field strength (B0) on the MRI-CEST contrast with the aim of comparing the in vivo CEST contrast detectability of these two agents in the glucoCEST procedure.MethodsPhosphate buffered solutions of D-Glucose or 3OMG (20 mM) were prepared at different pH values and Z-spectra acquired at several B1 levels and at 37°C. In vivo glucoCEST images were obtained at 3 T and 7 T over a period of 30 min after injection of D-Glucose or 3OMG (at the doses of 1.5 and 3 g/kg) in a murine melanoma tumour model.ResultsA markedly different pH dependence of CEST response was observed in vitro for D-Glucose and 3OMG. The glucoCEST contrast enhancement in the tumour region following the intravenous administration (at the dose 3 g/kg) resulted to be comparable for both the molecules: 1-2% at 3 T and 2-3% at 7 T. The ST% resulted almost constant for 3OMG over the 30 min period, whereas a significant increase in the case of D-Glucose was detected.ConclusionOur results show similar CEST contrast efficiency but different temporal kinetics for the metabolizable and the non-metabolizable glucose derivatives in tumour murine models when administered at the same doses.

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.

Faint Hα Emission in the Corona and Its Relation to the Prominences

1994 ◽  
Vol 144 ◽  
pp. 339-342
Author(s):  
V. N. Dermendjiev ◽  
Z. Mouradian ◽  
J.- L. Leroy ◽  
P. Duchlev
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Essential Role ◽  
Hα Emission

AbstractThe relation between episodically observed in the solar corona faint Hαemission structures and the long lived prominences was studied. Particular consideration was given for cases in which the corresponding prominences had undergone DB process. An MHD interpretation of the phenomenon “emissions froides” (cool emission) is proposed in which an essential role plays the prominence supporting magnetic field.

Sign in / Sign up

Export Citation Format

Share Document