Abstract
In this note, we begin by reviewing an argument (independent from 1304.6483) that the large AdS black holes dual to typical high-energy pure states of a single holographic CFT must have some structure at the horizon (i.e. a firewall/fuzzball). By weakly coupling the CFT to an auxiliary system, such a black hole can be made to evaporate. In a case where the auxiliary system is a second identical CFT, it is possible (for specific initial states) that the system evolves to precisely the thermofield double state as the original black hole evaporates. In this case, the dual geometry should include the "late-time" part of the eternal AdS black hole spacetime which includes smooth spacetime behind the horizon of the original black hole. Thus, we can say that the firewall evaporates. This provides a specific realization of the recent ideas of Maldacena and Susskind that the existence of smooth spacetime behind the horizon of an evaporating black hole can be enabled by maximal entanglement with a Hawking radiation system (in our case the second CFT) rather than prevented by it. For initial states which are not finely-tuned to produce the thermofield double state, the question of whether a late-time infalling observer experiences a firewall translates to a question about the gravity dual of a typical high-energy state of a two-CFT system.
Highlights
ΨΑ and in particular does not make reference to perturbative quantum field theory modes in the bulk
In this note, we begin by presenting an argument suggesting that large AdS black holes dual to typical high-energy pure states of a single holographic CFT must have some structure at the horizon, i.e. a fuzzball/firewall, unless the procedure to probe physics behind the horizon is state-dependent
In a case where the auxiliary system is a second identical CFT, it is possible that the system evolves to precisely the thermofield double state as the original black hole evaporates
Summary
Large black holes in Anti-de-Sitter space typically do not evaporate. They are in equilibrium with their Hawking radiation, which reaches the boundary of AdS and returns to the black hole in finite time. The first CFT in the state |ψ0 corresponds to a large AdS black hole microstate in a spacetime that is asymptotically global AdS This black hole is in equilibrium with its Hawking radiation. When we attach the wire, a localized region of the spatial boundary of this AdS space experiences a change in boundary conditions, and radiation begins to enter the spacetime from this region of the boundary This radiation gives rise to a gas of gravitons in AdS space, but eventually this collapses to form a black hole that grows in size. As we mentioned in the introduction, our argument here is closely related to the recent paper by Maldacena and Susskind [54]; the construction here provides a concrete example where entanglement between a black hole and its Hawking radiation can lead to smooth spacetime behind the horizon.
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