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The information paradox: conflicts and resolutions
High Energy Physics - Theory · Submitted 10 Jan 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Thus the evolution of radiation quanta with E ~ kT is modified by order unity at the horizon, and we resolve the information paradox.
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The abstract, sentence by sentence
Many relativists have been long convinced that black hole evaporation leads to information loss or remnants. String theorists have however not been too worried about the issue, largely due to a belief that the Hawking argument for information loss is flawed in its details. A recently derived inequality shows that the Hawking argument for black holes with horizon can in fact be made rigorous. What happens instead is that in string theory black hole microstates have no horizons. Thus the evolution of radiation quanta with E ~ kT is modified by order unity at the horizon, and we resolve the information paradox. We discuss how it is still possible for E >> kT objects to see an approximate black hole like geometry. We also note some possible implications of this physics for the early Universe.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Many relativists have been long convinced that black hole evaporation leads to information loss or remnants. | background 1.00 | 0.03 | 0.02 | asserted 0.67 |
| s1 | String theorists have however not been too worried about the issue, largely due to a belief that the Hawking argument for information loss is flawed in its details. | background 1.00 | 0.04 | 0.03 | asserted 0.82 |
| s2 | A recently derived inequality shows that the Hawking argument for black holes with horizon can in fact be made rigorous. | result 0.56 | 0.56 | 0.15 | asserted 0.99 |
| s3 | What happens instead is that in string theory black hole microstates have no horizons. | result 0.80 | 0.57 | 0.31 | asserted 1.00 |
| s4 | Thus the evolution of radiation quanta with E ~ kT is modified by order unity at the horizon, and we resolve the information paradox. | result 0.60 | 0.72 | 0.82 | asserted 1.00 |
| s5 | We discuss how it is still possible for E >> kT objects to see an approximate black hole like geometry. | result 0.32 | 0.53 | 0.05 | hedged possibility 0.87 |
| s6 | We also note some possible implications of this physics for the early Universe. | interpretation 0.80 | 0.59 | 0.03 | hedged possibility 0.79 |
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The paper
Original abstract
Many relativists have been long convinced that black hole evaporation leads to information loss or remnants. String theorists have however not been too worried about the issue, largely due to a belief that the Hawking argument for information loss is flawed in its details. A recently derived inequality shows that the Hawking argument for black holes with horizon can in fact be made rigorous. What happens instead is that in string theory black hole microstates have no horizons. Thus the evolution of radiation quanta with E ~ kT is modified by order unity at the horizon, and we resolve the information paradox. We discuss how it is still possible for E >> kT objects to see an approximate black hole like geometry. We also note some possible implications of this physics for the early Universe.
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References
How the literature uses it
22 arXiv papers cite this in 37 sentences
Papers citing it · 17 sentences without a confident label
Contests it 2 papers
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Lessons about the information paradox: We argued that, contrary to the claims of [ref] and [ref] , small corrections to the Hawking computation can restore unitarity.
An Infalling Observer in AdS/CFT · Conclusions and further directions · contest 0.89
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It is sometimes argued that fuzzballs are required to resolve the information paradox [ref] , and we explain, in section [ref], why we believe that this argument is incorrect.
A Critique of the Fuzzball Program · Introduction · contest 0.76
Cites it as support 3 papers
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For example, at its most basic level, the arguments of [ref] and the firewall argument indicate that information recovery requires a black hole to have a lot of hair at the horizon.
Resolving the Structure of Black Holes: Philosophizing with a Hammer · Introduction · 0.97
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Additionally, the astrophysical context indicated here (specifically, the presence of the CMB radiation) causes rapid decoherence, so entanglement across the horizon [ref] is rapidly lost [ref] and associated problems will therefore dematerialize.
Astrophysical black holes may radiate, but they do not evaporate · Theoretical Implications · 0.97
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First amongst these is Mathur's tightening [ref] of Hawking's result to show that information can only be recovered if there are $(1)$ corrections to the semi-classical physics outside black holes.
Black-Hole Entropy from Supergravity Superstrata States · Black-hole microstate structure · 0.96
Cites it as background 13 papers
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( [ref] , [ref] , [ref] , [ref] ).
On the paradox of Hawking radiation in a maximally extended Schwarzschild solution · Implications · 0.88
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Interest in black hole information [ref] has surged recently with the publication by Almheiri, Marolf, Polchinski, and Sully [ref] of a provocative argument that suggests that an “infalling observer burns up at the horizon” of a sufficiently old black hole, so that the horizon becomes what they called a “firewall.” This paper has elicited a large number of responses, some of which support the firewall idea [ref] , others seem rather agnostic [ref] , and yet others of which raise skepticism about it [ref] .
Time Dependence of Hawking Radiation Entropy · Introduction · 0.98
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( [ref] , [ref] , [ref] , [ref] ).
Astrophysical black holes may radiate, but they do not evaporate · Theoretical Implications · 0.95
What it cites · 37 sentences without a confident label
Compares with 1 paper
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(Note that the `fractional brane gas' is completely different from the traditional `brane gas' [ref] where we have essentially free (i.e. non-intersecting) branes with $S∼E$.)
Brane Gases in the Early Universe · Implications for Cosmology: a conjecture · 0.85
Cites as support 2 papers
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It turns out that no vibration profile generates a horizon; what happens instead is that in general we lose axial symmetry [ref] .
AdS/CFT duality and the black hole information paradox · Fuzzballs · 0.96
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(iii) The space of these gravitational `fuzzball' solutions can be quantized and shown to yield the entropy of the system [ref] .
D1-D5 black hole microstate counting from supergravity · Fuzzballs · 0.98
Cites as background 4 papers
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In 2005 Hawking himself conceded a long held bet with Preskill, arguing that small corrections from subleading saddle points in the Euclidean path-integral could remove the problem [ref] .
Information Loss in Black Holes · Introduction · 0.84
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A widespread belief in the string community was that the paradox has been bypassed in string theory because of the discovery of AdS/CFT duality [ref] .
The Large N Limit of Superconformal Field Theories and Supergravity · AdS/CFT duality · 0.93
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In the rest of this section we discuss the infall problem and the approximation in which we obtain the traditional geometry ([ref]).[For other related approaches to this problem, see [ref] .]
Black Holes as Effective Geometries · The infall problem · 0.94
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