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Holographic Schwinger-Keldysh effective field theories

Jan de Boer, Michal P. Heller, Natalia Pinzani-Fokeeva

Abstract

We construct a holographic dual of the Schwinger-Keldysh effective action for the dissipative low-energy dynamics of relativistic charged matter at strong coupling in a fixed thermal background. To do so, we use a mixed signature bulk spacetime whereby an eternal asymptotically anti-de Sitter black hole is glued to its Euclidean counterpart along an initial time slice in a way to match the desired double-time contour of the dual field theory. Our results are consistent with existing literature and can be regarded as a fully-ab initio derivation of a Schwinger-Keldysh effective action. In addition, we provide a simple infrared effective action for the near horizon region that drives all the dissipation and can be viewed as an alternative to the membrane paradigm approximation.

Holographic Schwinger-Keldysh effective field theories

Abstract

We construct a holographic dual of the Schwinger-Keldysh effective action for the dissipative low-energy dynamics of relativistic charged matter at strong coupling in a fixed thermal background. To do so, we use a mixed signature bulk spacetime whereby an eternal asymptotically anti-de Sitter black hole is glued to its Euclidean counterpart along an initial time slice in a way to match the desired double-time contour of the dual field theory. Our results are consistent with existing literature and can be regarded as a fully-ab initio derivation of a Schwinger-Keldysh effective action. In addition, we provide a simple infrared effective action for the near horizon region that drives all the dissipation and can be viewed as an alternative to the membrane paradigm approximation.

Paper Structure

This paper contains 16 sections, 111 equations, 3 figures.

Figures (3)

  • Figure 1: The Schwinger-Keldysh contour at finite temperature. Time flows forward from $t=0$ to $t=+\infty$ and back to where the initial state is defined. The latter is represented by an imaginary time segment identified along the circles with period $\beta=1/T$.
  • Figure 2: On the left-hand side (a): an eternal AdS black hole where the arrows indicate the flow of time. We cut along the an initial time slice at $t=0$ and a late time slice at $t=\hat{t}$ (dashed lines), and we keep the region in between them. On the right-hand side (b): a Euclidean black hole in AdS with period $\beta$. We cut along finite time slices at $\tau=0$ and $\tau = \beta-\sigma$ (dashed lines). For simplicity we have depicted the spacetimes in $2+1$ dimensions in the global time and radial coordinate.
  • Figure 3: The mixed signature bulk spacetime containing two Lorentzian regions, ${\cal M}_R$ and ${\cal M}_L$, with future horizons identified and one Euclidean black hole ${\cal M}_E$ glued smoothly together along finite time slices. Notice that in order to simplify the drawing we flipped the left segment with respect to the way it appears in fig. \ref{['fig.spacetime']}, so that the left time increases now upwards.