Soliton theory of superconducting transitions

2021 ◽  
Author(s):  
Minoru Fujimoto
Keyword(s):  
Soliton Theory ◽  
Superconducting Transitions

scholarly journals The Superconducting Critical Temperature

Symmetry ◽  
2021 ◽  
Vol 13 (5) ◽  
pp. 911
Author(s):  
Mike Guidry ◽  
Yang Sun ◽  
Lian-Ao Wu
Keyword(s):  
Critical Temperature ◽  
Dynamical Symmetry ◽  
Many Body ◽  
Unconventional Superconductors ◽  
The Many ◽  
Pair Coupling ◽  
Intrinsic Strength ◽  
Superconducting Transitions

Two principles govern the critical temperature for superconducting transitions: (1) intrinsic strength of the pair coupling and (2) the effect of the many-body environments on the efficiency of that coupling. Most discussions take into account only the former, but we argue that the properties of unconventional superconductors are governed more often by the latter, through dynamical symmetry relating to normal and superconducting states. Differentiating these effects is essential to charting a path to the highest-temperature superconductors.

FIRST-ORDER APPROXIMATION OF THE NUMBER-PROJECTED SO(2N) TAMM-DANCOFF EQUATION AND ITS REDUCTION BY THE SCHUR FUNCTION

1999 ◽  
Vol 08 (05) ◽  
pp. 461-483
Author(s):  
SEIYA NISHIYAMA
Keyword(s):  
Wave Function ◽  
Order Approximation ◽  
Approximate Equation ◽  
Variation Principle ◽  
Schur Function ◽  
Soliton Theory ◽  
First Order ◽  
Fermion Systems ◽  
Group Manifold ◽  
First Order Approximation

First-order approximation of the number-projected (NP) SO(2N) Tamm-Dancoff (TD) equation is developed to describe ground and excited states of superconducting fermion systems. We start from an NP Hartree-Bogoliubov (HB) wave function. The NP SO(2N) TD expansion is generated by quasi-particle pair excitations from the degenerate geminals in the number-projected HB wave function. The Schrödinger equation is cast into the NP SO(2N) TD equation by the variation principle. We approximate it up to first order. This approximate equation is reduced to a simpler form by the Schur function of group characters which has a close connection with the soliton theory on the group manifold.

Quantum interference and superconducting transitions in 2D

Physica B+C ◽  
1981 ◽  
Vol 107 (1-3) ◽  
pp. 489-490 ◽  
Author(s):  
R.H. Cantor ◽  
A.M. Goldman
Keyword(s):  
Quantum Interference ◽  
Superconducting Transitions

Soliton theory of squall storms

2010 ◽  
Vol 65 (5) ◽  
pp. 412-416 ◽  
Author(s):  
S. A. Arsen’ev ◽  
N. K. Shelkovnikov
Keyword(s):  
Soliton Theory

Nonmonotonic superconducting transitions in mesoscopic Al structures induced by radio-frequency radiation

1996 ◽  
Vol 53 (17) ◽  
pp. 11332-11335 ◽  
Author(s):  
C. Strunk ◽  
V. Bruyndoncx ◽  
C. Van Haesendonck ◽  
V. V. Moshchalkov ◽  
Y. Bruynseraede ◽  
...  
Keyword(s):  
Radio Frequency ◽  
Radio Frequency Radiation ◽  
Frequency Radiation ◽  
Superconducting Transitions

scholarly journals Isometric immersions of space forms and soliton theory

1996 ◽  
Vol 305 (1) ◽  
pp. 329-342 ◽  
Author(s):  
Dirk Ferus ◽  
Franz Pedit
Keyword(s):  
Isometric Immersions ◽  
Space Forms ◽  
Soliton Theory

Topics in soliton theory

1992 ◽  
Vol 34 (2) ◽  
pp. 184
Author(s):  
W.F. Ames ◽  
C. Brezinski
Keyword(s):  
Soliton Theory

scholarly journals Magnetic holes in the solar wind between 0.3 AU and 17 AU

2000 ◽  
Vol 7 (3/4) ◽  
pp. 191-200 ◽  
Author(s):  
K. Sperveslage ◽  
F. M. Neubauer ◽  
K. Baumgärtel ◽  
N. F. Ness
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Heliocentric Distance ◽  
Occurrence Rate ◽  
Automatic Identification ◽  
Soliton Theory ◽  
Theoretical Approaches ◽  
Maximum Angle ◽  
Using Data ◽  
Initial Magnetic Field

Abstract. Magnetic holes (MHs) are depressions of the magnetic field magnitude. Turner et al. (1977) identified the first MHs in the solar wind and determined an occurrence rate of 1.5 MHs/d. Winterhalter et al. (1994) developed an automatic identification criterion to search for MHs in Ulysses data in the solar wind between 1 AU and 5.4 AU. We adopt their criterion to expand the search to the heliocentric distances down to 0.3 AU using data from Helios 1 and 2 and up to 17 AU using data from Voyager 2. We relate our observations to two theoretical approaches which describe the so-called linear MHs in which the magnetic vector varies in magnitude rather than direction. Therefore we focus on such linear MHs with a directional change less than 10º. With our observations of about 850 MHs we present the following results: Approximately 30% of all the identified MHs are linear. The maximum angle between the initial magnetic field vector and any vector inside the MH is 20º in average and shows a weak relation to the depth of the MHs. The angle between the initial magnetic field and the minimum variance direction of those structures is large and very probably close to 90º. The MHs are placed in a high β environment even though the average solar wind shows a smaller β. The widths decrease from about 50 proton inertial length in a region between 0.3 AU and 0.4 AU heliocentric distance to about 15 proton inertial length at distances larger than 10 AU. This quantity is correlated with the β of the MH environments with respect to the heliocentric distance. There is a clear preference for the occurrence of depressions instead of compressions. We discuss these results with regard to the main theories of MHs, the mirror instability and the alternative soliton approach. Although our observational results are more consistent with the soliton theory we favour a combination of both. MHs might be the remnants of initial mirror mode structures which can be described as solitons during the main part of their lifetime.

Sign in / Sign up

Export Citation Format

Share Document