Abstract
We study the quasinormal modes and thermal radiation of massless spin-0 field perturbations in the background of four-dimensional (4D) non-Abelian charged Lifshitz black branes with z=2 hyperscaling violation, which correspond to systems with superconducting fluctuations. After having an analytical solution to the Klein–Gordon equation, we obtain exact quasinormal modes that are purely imaginary. Therefore, there is no oscillatory behavior in the perturbations that guarantees the mode stability of these solutions. We also study the greybody factors, absorption cross-section, and decay rate of the non-Abelian charged Lifshitz black branes. We derive their analytical expressions and then investigate the correspondence in the strongly coupled dual theory. This study might shed light on the mechanism governing the high-temperature superconductors in condensed matter physics.
Highlights
15] and in string theory [16,17]
The quasinormal modes (QNMs), on the other hand, disclose how quick a thermal state in the boundary theory will reach thermal equilibrium according to the AdS/CFT correspondence [55]
This happens because the relaxation time of a thermal state is inversely proportional to the imaginary part of the QNMs of the dual gravity background that was achieved by the QNMs of the bulk spacetime, which appears from the poles of the retarded correlation function of the corresponding perturbations of the dual CFT [56]
Summary
For strongly-coupled systems in holographic CM physics, ’t Hooft matrix large N limit needs to be taken into account. In which λ denotes ’t Hooft coupling and for the cases when λ is large, strong interactions occur. During this study, based on our current literature knowledge, we have seen that it is not possible to obtain the exact analytical solution of the generic radial equation (9) due to its transcendental form. The general solution for the radial function is obtained as (z) = zα(1 − z)β C1 2 F1 (a, b; c; z) +C2 z1−c 2 F1 (a − c + 1, b − c + 1; 2 − c; z) After this point, one shall split the problem into two parts and investigate the behavior of Eq (28) near the event horizon and at the spatial infinity regime separately. This will provide the desired information regarding the flux computation
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