Falling Toward Charged Black Holes

TL;DR

The paper analyzes scrambling in near-extremal charged black holes using a size–momentum duality, where the growth of operator size is tied to the momentum of an infalling wave packet through the RN throat. By introducing a position-dependent local energy scale along the throat, the authors show that operator size undergoes rapid early growth (quadratic in time) before entering the exponential growth phase in the Rindler region, yielding a scrambling time $\tau_* = \log\left(\frac{S-S_0}{\delta S}\right)$. This explains the reduced scrambling time relative to neutral black holes not as a decoupling of extremal degrees of freedom, but as a consequence of the throat dynamics accelerating the precursor. The results align with SYKModel predictions at finite temperature, supporting a GR=QM viewpoint and highlighting a universal, geometry-driven mechanism for scrambling across neutral and charged horizons.

Abstract

The growth of the "size" of operators is an important diagnostic of quantum chaos. In arXiv:1802.01198 [hep-th] it was conjectured that the holographic dual of the size is proportional to the average radial component of the momentum of the particle created by the operator. Thus the growth of operators in the background of a black hole corresponds to the acceleration of the particle as it falls toward the horizon. In this note we will use the momentum-size correspondence as a tool to study scrambling in the field of a near-extremal charged black hole. The agreement with previous work provides a non-trivial test of the momentum-size relation, as well as an explanation of a paradoxical feature of scrambling previously discovered by Leichenauer [arXiv:1405.7365 [hep-th]]. Naively Leichenauer's result says that only the non-extremal entropy participates in scrambling. The same feature is also present in the SYK model. In this paper we find a quite different interpretation of Leichenauer's result which does not have to do with any decoupling of the extremal degrees of freedom. Instead it has to do with the buildup of momentum as a particle accelerates through the long throat of the Reissner-Nordstrom geometry.

Figures (1)

• Figure 1: The three regions outside a near-extremal charged black hole. Unlike for uncharged black holes, there is now a 'throat' separating the Rindler and Newtonian regions.