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arXiv:2510.18967 · Physical review. D/Physical review. D.

Stabilizer complexity of Hawking radiation

Anonymous, Onkar Parrikar, Suprakash Paul, Harshit Rajgadia

Published Jul 13, 2026• 2 citations
arXivHTMLPDF

Abstract

We study the complexity of Hawking radiation for an evaporating black hole from the perspective of the stabilizer theory of quantum computation. Specifically, we calculate Wigner negativity—a magic monotone that can be interpreted as a measure of the stabilizer complexity, or equivalently, the complexity of classical simulation—in various toy models for evaporating black holes. We first calculate the Wigner negativity of Hawking radiation in the Penington-Shenker-Stanford-Yang (PSSY) model directly using the gravitational path integral, and show that the negativity is O ( 1 ) before the Page transition, but becomes exponentially large past the Page transition. We also derive a universal, information theoretic formula for the negativity that interpolates between the two extremes. We then study the Wigner negativity of radiation in a dynamical model of black hole evaporation. In this case, the negativity shows a sharp spike at early times resulting from the coupling between the black hole and the radiation system, but at late times when the system settles down, we find that the negativity satisfies the same universal formula as in the PSSY model. Finally, we also propose a geometric formula for Wigner negativity in general holographic states using intuition from fixed area states and random tensor networks, and argue that a python’s lunch in the entanglement wedge implies a stabilizer complexity that is exponentially large in 1 8 G N times the difference between the areas corresponding to the outermost and minimal extremal surfaces.

DOI
10.1103/49df-l9n4

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We study the complexity of Hawking radiation for an evaporating black hole from the perspective of the stabilizer theory of quantum computation. Specifically, we calculate Wigner negativity—a magic monotone that can be interpreted as a measure of the stabilizer complexity, or equivalently, the complexity of classical simulation—in various toy models for evaporating black holes. We first calculate the Wigner negativity of Hawking radiation in the Penington-Shenker-Stanford-Yang (PSSY) model directly using the gravitational path integral, and show that the negativity is O ( 1 ) before the Page transition, but becomes exponentially large past the Page transition. We also derive a universal, information theoretic formula for the negativity that interpolates between the two extremes. We then study the Wigner negativity of radiation in a dynamical model of black hole evaporation. In this case, the negativity shows a sharp spike at early times resulting from the coupling between the black hole and the radiation system, but at late times when the system settles down, we find that the negativity satisfies the same universal formula as in the PSSY model. Finally, we also propose a geometric formula for Wigner negativity in general holographic states using intuition from fixed area states and random tensor networks, and argue that a python’s lunch in the entanglement wedge implies a stabilizer complexity that is exponentially large in 1 8 G N times the difference between the areas corresponding to the outermost and minimal extremal surfaces.
In this note, we study the stabilizer complexity of the reduced density matrix corresponding to one side of a partially entangled thermal (PET) state with fixed energy boundary conditions in a holographic CFT. In particular, we study Wigner negativity, an operationally meaningful magic monotone which can be interpreted as the complexity of classically simulating any quantum circuit preparation of the reduced state on the subregion. Using assumptions on the pseudorandomness of the CFT spectrum and the heavy operator insertion, we observe that the Wigner negativity of the PET state relative to the microcanonical density matrix at the given energy is given by exp⁡[18GN(Aout−Amin)]\exp\left[\frac{1}{8G_N}(A_{\text{out}} - A_{\text{min}})\right]exp[8GN​1​(Aout​−Amin​)], where AoutA_{\text{out}}Aout​ is the area of the outer extremal surface, while AminA_{\text{min}}Amin​ is the area of the minimal extremal surface. Thus, the stabilizer complexity of the reduced density matrix on the boundary subregion is O(1)O(1)O(1) in the absence of a python's lunch, but gets exponentially enhanced in the presence of a python's lunch in the bulk geometry.
A bstract According to Harlow and Hayden [ arXiv:1301.4504 ] the task of distilling information out of Hawking radiation appears to be computationally hard despite the fact that the quantum state of the black hole and its radiation is relatively un-complex. We trace this computational difficulty to a geometric obstruction in the Einstein-Rosen bridge connecting the black hole and its radiation. Inspired by tensor network models, we conjecture a precise formula relating the computational hardness of distilling information to geometric properties of the wormhole — specifically to the exponential of the difference in generalized entropies between the two non-minimal quantum extremal surfaces that constitute the obstruction. Due to its shape, we call this obstruction the ‘Python’s Lunch’, in analogy to the reptile’s postprandial bulge.
Abstract We construct a holographic map that takes the semi-classical state of an evaporating black hole and its Hawking radiation to a microscopic model that reflects the scrambling dynamics of the black hole. The microscopic model is given by a nested sequence of random unitaries, each one implementing a scrambling time step of the black hole evolution. Differently from other models, energy conservation and the thermal nature of the Hawking radiation are taken into account. We show that the QES formula follows for the entropy of multiple subsets of the radiation and black hole. We further show that a version of entanglement wedge reconstruction can be proved by computing suitable trace norms and quantum fidelities involving the action of a unitary on a subset of Hawking partners. If the Hawking partner is in an island, its unitary can be reconstructed by a unitary on the radiation. We also adopt a similar setup and analyse reconstruction of unitaries acting on an infalling system.
A bstract We investigate the simple model of Pennington, Shenker, Stanford and Yang for modeling the density matrix of Hawking radiation, but further include dynamics for EOW branes behind the horizon. This allows interactions that scatter one interior state to another, and also allows EOW loops. At strong coupling, we find that EOW states are no longer random; the ensemble has collapsed, and coupling constants encode the microscopic matrix elements of Hawking radiation. This suggests strong interior dynamics are important for understanding evaporating black holes, without any ensemble average. In this concrete model the density matrix of the radiation deviates from the thermal state, small off-diagonal fluctuations encode equivalences between naively orthogonal states, and bound the entropy from above. For almost evaporated black holes the off-diagonal terms become as large as the diagonal ones, eventually giving a pure state. We also find the unique analytic formula for all Renyi entropies.
We investigate a plausible route to resolving the black hole information paradox by examining the effects of decoherence on Hawking radiation. In particular, we show that a finite but nonzero rate of decoherence can lead to efficient extraction of information from the evaporating black hole. This effectively pushes the paradox from becoming manifest at the Page time when the black hole has evaporated to half its size, to a timescale solely determined by the rate of decoherence. If this rate is due to a putative interaction with gravitons, the black hole at this timescale can be expected to be Planck sized, but notably without an extensive amount of information packed inside. We justify our findings by numerically studying a toy model of stabilizer circuits that can efficiently model black hole evaporation in the presence of decoherence. The latter is found to be well described by an effective rate equation for the entanglement and which corroborates our findings.
This thesis studies the complexity, thermalization, and entanglement properties of quantum mechanical systems and the implications of their behavior in high energy and condensed matter models. In Chapter 2, we use the geometry of Lie groups to study the circuit complexity of quantum mechanical systems and develop the technology to analytically predict the appearance of the obstruction to the complexity growth of integrable systems. We simulate the spin and fermionic systems, in which the amount of chaos can be controlled, and conjecture the close relation between quantum complexity and thermalization. In Chapter 3, we apply quantum information theory to an evaporating black hole in Jackiw-Teitelboim gravity in the context of AdS/CFT as a quantum error correction protocol. By calculating the entropy measures using gravitational path integrals, we establish the criterion for an error in the Hawking radiation to be correctable and identify the transition in the reversibility of the error channel as the Page transition. In Chapter 4, we study a 1+1 dimensional random circuit with measurement and dissipation. We map this type of quantum system to a classical Ising model analytically and show that the entanglement dynamics can be understood as the thermodynamics of the domain wall formed in the spin model, as one of the spatial dimensions stretches. We then confirm the calculated time scales in the classical theory qualitatively with simulations of realistic qubit circuits. Overall, we present a holistic picture of quantum systems, from those evolving with pure unitary, to those evolving also with influence from the environment. The complexity of the theory and entanglement of the states exhibit universal behavior at early times (∼ O(N)) and distinct long-time behavior, determined by their thermalization properties in spin chains, toy models of black holes in AdS/CFT, and monitored random circuits with dissipation.