What does strong subadditivity tell us about black holes?

Abstract

It has been argued that small corrections to evolution arising from non-geometric effects can resolve the information paradox. We can get such effects, for example, from subleading saddle points in the Euclidean path integral. But an inequality derived in 2009 using strong sub-additivity showed that such corrections {\it cannot} solve the problem. As a result we sharpen the original Hawking puzzle: we must either have (A) new (nonlocal) physics or (B) construct hair at the horizon. We get correspondingly different approaches to resolving the AMPS puzzle. Traditional complementarity assumes (A); here we require that the AMPS experiment measures the correct vacuum entanglement of Hawking modes, and invoke nonlocal $A=R_B$ type effects to obtain unitarity of radiation. Fuzzball complementarity is in category (B); here the AMPS measurement is outside the validity of the approximation required to obtain the complementary description, and a effective regular horizon arises only for freely infalling observers with energies $E\gg T$.

12 pages, 8 figures, Expanded version of proceedings for Light Cone 2012, Delhi

References in corpus (6)

• Gravity solutions for the D1-D5 system with angular momentum
• Global Structure of Five-dimensional BPS Fuzzballs
• The flaw in the firewall argument
• Passing through the Firewall
• What the information paradox is {\it not}
• Black Hole Information as Topological Qubits

Cited by in corpus (18)

• State-Dependent Bulk-Boundary Maps and Black Hole Complementarity
• Comments on the Necessity and Implications of State-Dependence in the Black Hole Interior
• Excluding Black Hole Firewalls with Extreme Cosmic Censorship
• Black holes as collapsed polymers
• When black holes collide: Probing the interior composition by the spectrum of ringdown modes and emitted gravitational waves
• Resisting collapse: How matter inside a black hole can withstand gravity
• Discovering the interior of black holes
• Non-singular black holes interiors need physics beyond the standard model
• Smooth Causal Patches for AdS Black Holes
• Quantum state of the black hole interior
• Emergent horizon, Hawking radiation and chaos in the collapsed polymer model of a black hole
• The state of Hawking radiation is non-classical
• Density matrix of black hole radiation
• Falling through the black hole horizon
• The Firewall Paradox
• Constraints on the quantum state of pairs produced by semiclassical black holes
• Tunneling across the quantum horizon does not resolve the information paradox
• Teleporting entanglement during black hole evaporation