scholarly journals Granular superconductivity and magnetic-field-driven recovery of macroscopic coherence in a cuprate/manganite multilayer

2016 ◽  
Vol 94 (18) ◽  
Author(s):  
B. P. P. Mallett ◽  
J. Khmaladze ◽  
P. Marsik ◽  
E. Perret ◽  
A. Cerreta ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Granular Superconductivity

SUPERCONDUCTIVITY ASSOCIATED WITH THE GRANULAR STRUCTURE IN Ba2YCu3O7−δ

1988 ◽  
Vol 02 (08) ◽  
pp. 1011-1015
Author(s):  
YONG ZHAO ◽  
QIRUI ZHANG ◽  
WEIYAN GUAN ◽  
JIANSHENG XIA ◽  
ZHENHUI HE ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Transport Properties ◽  
Single Phase ◽  
Granular Structure ◽  
Current Voltage ◽  
Granular Superconductivity ◽  
Current Voltage Characteristics ◽  
The Magnetic Field ◽  
Nonmonotonic Behavior

The dependence of the resistance on the magnetic field and the current-voltage characteristics of the single phase Ba 2 YCu 3 O 7−δ have been measured. The nonmonotonic behavior and a hysteresis of R(H) and the current-voltage characteristics suggest that the granular superconductivity exist in this material, and it plays an important role in transport properties.

TEMPERATURE DEPENDENCE OF THE QUANTUM INTERFERENCE PERIODICITY OF HIGH-TEMPERATURE SUPERCONDUCTIVE MATERIAL

1991 ◽  
Vol 05 (16) ◽  
pp. 1105-1108
Author(s):  
C. X. FAN ◽  
K. W. WONG
Keyword(s):  
Magnetic Field ◽  
High Temperature ◽  
Temperature Dependence ◽  
Linear Relationship ◽  
Field Dependence ◽  
Quantum Interference ◽  
Magnetic Field Dependence ◽  
Temperature Sensitive ◽  
Network System ◽  
Granular Superconductivity

The property of periodic magnetic field dependence observed on high temperature material is temperature sensitive. Experimental results show a linear relationship between τ2 and T4, where τ is the rf quantum interference period and T is temperature. This relation emerge from the entirety of weaklinks network system of granular superconductivity.

scholarly journals Transport characteristics of focused beam deposited nanostructures

2015 ◽  
Vol 2 (1) ◽  
Author(s):  
Ana Ballestar ◽  
Pablo Esquinazi
Keyword(s):  
Magnetic Field ◽  
Electron Beam ◽  
Transport Properties ◽  
Hysteresis Loops ◽  
Variable Range Hopping ◽  
Electron Beam Deposition ◽  
Granular Superconductivity ◽  
Metallic Grains ◽  
Focused Beam ◽  
Beam Deposition

AbstractWe review the transport properties of different nanostructures produced by ion- and electron-beam deposition, as prepared as well as after certain treatments. In general, the available literature indicates that the transport properties are determined by conduction processes typical for disordered metallic grains embedded in a carbon-rich matrix, including intergrain tunneling and variable range hopping mechanisms. Special emphasis is given to the superconducting behavior found in certain Tungsten-Carbide nanostructures that, in a certain field and temperature range, is compatible with that of granular superconductivity. This granular superconductivity leads to phenomena like magnetic field oscillations as well as anomalous hysteresis loops in the magnetoresistance.

BEHAVIOUR OF ORIENTED POLYCRYSTALLINE YBaCuO SUPERCONDUCTING THIN FILMS IN A WEAK MAGNETIC FIELD

1990 ◽  
Vol 04 (15) ◽  
pp. 975-982
Author(s):  
H.H. WEN ◽  
X.W. CAO ◽  
J.Z. SHI ◽  
W.Z. SHI ◽  
W.G. YAO ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Thin Films ◽  
Critical Field ◽  
Weak Magnetic Field ◽  
Flow Resistance ◽  
Weak Links ◽  
Superconducting Thin Films ◽  
Flux Flow ◽  
Granular Superconductivity ◽  
Oriented Polycrystalline

We determined a few characteristics of granular superconductivity through magnetoresistance measurements made on oriented polycrystalline YBaCuO superconducting thin films, and found that, at 77.3 K, the critical field for breaking a major portion of the superconducting weak links between grains was about 80 G, while the average lower critical field of the grains was about 175 G. Detail analyses on flux flow resistance show that a maximum of the increasing of flux flow resistance induced by a unit field will exist at a specified temperature, which we think is related to the dependence of the pinning energy on the temperature.

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.

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.

Sign in / Sign up

Export Citation Format

Share Document