On the gauge-invariant description of the evolution equations integrable by Gelfand-Dikij spectral problems

1982 ◽  
Vol 92 (7) ◽  
pp. 323-327 ◽  
Author(s):  
B.G. Konopelchenko
2020 ◽  
Vol 23 (3) ◽  
pp. 338-341
Author(s):  
Sergei Sakovich

The gauge-invariant description of zero-curvature representations of evolution equations is applied to the problem of how to distinguish the fake Lax pairs from the true Lax pairs. The main difference between the true Lax pairs and the fake ones is found in the structure of their cyclic bases.


2021 ◽  
Vol 2021 (6) ◽  
Author(s):  
Song He ◽  
Zhenjie Li ◽  
Qinglin Yang

Abstract We study cluster algebras for some all-loop Feynman integrals, including box-ladder, penta-box-ladder, and double-penta-ladder integrals. In addition to the well-known box ladder whose symbol alphabet is $$ {D}_2\simeq {A}_1^2 $$ D 2 ≃ A 1 2 , we show that penta-box ladder has an alphabet of D3 ≃ A3 and provide strong evidence that the alphabet of seven-point double-penta ladders can be identified with a D4 cluster algebra. We relate the symbol letters to the u variables of cluster configuration space, which provide a gauge-invariant description of the cluster algebra, and we find various sub-algebras associated with limits of the integrals. We comment on constraints similar to extended-Steinmann relations or cluster adjacency conditions on cluster function spaces. Our study of the symbol and alphabet is based on the recently proposed Wilson-loop d log representation, which allows us to predict higher-loop alphabet recursively; by applying it to certain eight-point and nine-point double-penta ladders, we also find D5 and D6 cluster functions respectively.


1990 ◽  
Vol 238 (2-4) ◽  
pp. 373-379 ◽  
Author(s):  
Stefano Catani ◽  
Emilio D'Emilio

1991 ◽  
Vol 06 (12) ◽  
pp. 2075-2108 ◽  
Author(s):  
ROBERT K. SCHAEFER

Formulas are derived for describing the evolution of fluctuations in the density of collisionless particles in the expanding universe using the gauge-invariant fluid description. The formulas use the “gauge-invariant” variables proposed by Bardeen to describe cosmological perturbations. These variables are hydrodynamic in nature and we show the behavior of the equations when the particles have streaming lengths large compared to the scales of interest. We also show how these equations couple gravitationally when other species of matter are present in significant densities. Using the “fourteen moment” approximation for the particle distribution function, we get a simple set of ordinary differential equations which are much easier to use than a direct integration of the Boltzmann equation. This formulation is especially useful when we are considering universes with more than one cosmologically significant component of matter density. An example of a numerical integration of the evolution equations is presented for comparison of this method to other work. A formula for calculating fluctuations in the cosmic microwave background radiation is also given.


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