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arxiv: 2411.01105 · v2 · submitted 2024-11-02 · ✦ hep-th

UV Effects and Short-Lived Hawking Radiation: Alternative Resolution of Information Paradox

Pei-Ming Ho , Hikaru Kawai , Wei-Hsiang Shao This is my paper

Pith reviewed 2026-05-23 18:04 UTC · model grok-4.3

classification ✦ hep-th
keywords black hole information paradoxHawking radiationstring theoryUV effectsscrambling timegeneralized uncertainty principletrans-Planckian effects
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The pith

Hawking radiation terminates around the scrambling time due to trans-Planckian stringy effects, leaving black holes mostly classical.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper proposes that trans-Planckian effects inherent in string theory cause Hawking radiation to cease around the scrambling time. Two toy models are examined: one using the generalized uncertainty principle to introduce a minimal length, and another inspired by string field theory with exponential suppression of UV interactions. Both models show that radiation stops early, so evaporated energy remains negligible and the black hole stays predominantly classical. This offers an alternative resolution to the information paradox because little radiation escapes and no complex recovery of interior information is required. A reader would care because the claim relies only on standard string theory features rather than new horizon-scale physics.

Core claim

The central claim is that Hawking radiation ceases around the scrambling time due to trans-Planckian effects in string theory. The two toy models—one with a generalized uncertainty principle introducing minimal length and one with exponential UV suppression from string field theory—both indicate early termination, resulting in negligible evaporated energy and a predominantly classical black hole.

What carries the argument

Early termination of Hawking radiation triggered by UV suppression in the generalized uncertainty principle and string-field-theory-inspired exponential cutoff models.

Load-bearing premise

The two toy models correctly capture the trans-Planckian effects that would terminate Hawking radiation at the scrambling time in a real string-theoretic black hole.

What would settle it

A calculation or observation showing that Hawking radiation from a black hole continues with significant energy loss well beyond the scrambling time would falsify the claim.

Figures

Figures reproduced from arXiv: 2411.01105 by Hikaru Kawai, Pei-Ming Ho, Wei-Hsiang Shao.

Figure 1
Figure 1. Figure 1: Panel (a) shows the Penrose diagram of a black hole in the traditional model and panel (b) that of a classical black hole. The shaded areas refer to the regions beyond a certain cutoff retarded time. We will only be concerned with Hawking radiation before this cutoff time, which will later be identified as the scrambling time. Causally, the region above the cutoff time cannot affect the Hawking radiation b… view at source ↗
Figure 2
Figure 2. Figure 2: In terms of the Eddington retarded time u, which agrees with the Schwarzschild time t at a fixed radius r, the time for a black hole to evaporate to 1% of its initial mass M is O(a 3/ℓ2 p ). However, in terms of the proper time of a comoving observer, this process occurs over a brief time scale ∼ 1000ℓp [69]. on the areal radius r. Due to the negative ingoing energy flux, the outer trapping horizon is time… view at source ↗
Figure 3
Figure 3. Figure 3: Illustration of nice slices that intersects the infalling matter and both early and late Hawking radiation. 2.2.5 Nice Slices Away from the singularity, the spacetime geometry of a large black hole is smooth. It is possible to construct time slices in the Schwarzschild space (see fig. 3) such that the extrinsic and intrinsic curvatures remain small (∼ O(1/a)) until the black hole becomes microscopic. These… view at source ↗
Figure 4
Figure 4. Figure 4: Since the Unruh vacuum is a pure state, Hawking particles outside the horizon are entangled with their partners inside the horizon. Hence, the entanglement entropy of the black hole (blue curve) increases over time. On the other hand, the Bekenstein-Hawking entropy (red curve) decreases as the black hole evaporates. There is a conflict at the Page time when the entanglement entropy of the black hole become… view at source ↗
Figure 5
Figure 5. Figure 5: A thin null shell with a flat interior collapses to form a black hole. The calculation of Hawking radiation involves tracing an outgoing wave packet backward in time and decomposing it in terms of the Minkowski modes inside the shell. the Klein-Gordon inner product on a constant-v hypersurface of this background can be ex￾pressed as ⟨ϕ1 , ϕ2⟩ ≡ −i Z ∞ −∞ dx ϕ∗ 1 (v, x) ↔ ∂x ϕ2(v, x) = 2 Z ∞ −∞ dp Φ ∗ 1 (v,… view at source ↗
Figure 6
Figure 6. Figure 6: A graph illustrating the positive-p branch of the characteristic trajectory v − u0 = −2aF(p) (5.30) (solid blue curve), alongside its counterpart in the low-energy theory (dashed black curve). Arrows indicate the flow direction toward the past (decreasing v). With the introduction of the GUP, the momentum reaches infinity in a finite time marked by the dotted red line. Based on these results, a Hawking par… view at source ↗
Figure 7
Figure 7. Figure 7: A schematic illustration of a high-frequency outgoing wave packet with a narrow width ∆U. The wave packet behaves like an extended string spanning a range ∆V > 4ℓ 2 s/∆U. The vertical line represents the worldvolume of matter that eventually collapses into a black hole with a size considerably smaller than ∆V . Since the wave packet cannot be localized near the horizon, it does not contribute to Hawking ra… view at source ↗
Figure 8
Figure 8. Figure 8: Panel (a) shows the Penrose diagram of a black hole with Hawking radiation terminated at an early stage marked by the dashed red line. The background is defined in the low-energy limit. While the spacetime metric may not be well-defined for trans-Planckian modes, panel (b) schematically illustrates the Penrose diagram of a highly smeared black-hole geometry, representing the background on which the vacuum … view at source ↗
read the original abstract

This chapter suggests an alternative solution to the black-hole information paradox by proposing that Hawking radiation ceases around the scrambling time due to trans-Planckian effects inherent in string theory. We consider two toy models in the literature that incorporate stringy effects. The first model utilizes the generalized uncertainty principle, which introduces a minimal length. The second model is inspired by string field theory, where interactions are exponentially suppressed in the UV limit. Both models indicate an early termination of Hawking radiation around the scrambling time, resulting in negligible evaporated energy and a predominantly classical black hole.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The manuscript claims that trans-Planckian effects in string theory cause Hawking radiation to terminate around the scrambling time. Two toy models are considered: the generalized uncertainty principle with a minimal length, and an exponential UV suppression inspired by string field theory. Both are said to produce early termination, negligible total evaporated energy, and a predominantly classical black hole, thereby offering an alternative resolution to the information paradox.

Significance. If the models were shown via explicit recomputation of the evaporation integral or modified Bogoliubov coefficients to terminate radiation precisely at t_scr rather than at an arbitrary cutoff scale, the result would supply a concrete mechanism limiting quantum effects to a short epoch. The approach reuses standard UV-cutoff constructions, so its significance rests entirely on whether the timing emerges as an output rather than an input.

major comments (2)
  1. The central claim requires that the GUP minimal-length and string-field exponential-suppression models produce a Hawking flux that drops to negligible levels specifically by the scrambling time t_scr ~ r_s log(r_s/l_p). The abstract and available description give no indication that modified mode equations or the full evaporation integral have been recomputed; the termination time therefore remains an input set by the cutoff parameters rather than a derived output.
  2. The two models contain free parameters (minimal length scale in the GUP model; UV suppression parameter in the string-field-theory model) that directly set the scale at which radiation is suppressed. The manuscript must demonstrate that the claimed termination at the scrambling time is robust under reasonable variations of these parameters or is fixed by an independent string-theoretic argument.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments. We clarify below that the termination arises from the string-scale cutoffs in the toy models and address the concerns about derivation versus input and parameter robustness.

read point-by-point responses

  1. Referee: The central claim requires that the GUP minimal-length and string-field exponential-suppression models produce a Hawking flux that drops to negligible levels specifically by the scrambling time t_scr ~ r_s log(r_s/l_p). The abstract and available description give no indication that modified mode equations or the full evaporation integral have been recomputed; the termination time therefore remains an input set by the cutoff parameters rather than a derived output.

    Authors: The models incorporate UV cutoffs at the string/Planck scale that suppress the flux once emitted frequencies become trans-Planckian. The time at which this occurs for the relevant near-horizon modes is identified with t_scr via the logarithmic redshift factor. We agree that an explicit recomputation of the modified Bogoliubov coefficients and the integrated evaporation rate would strengthen the presentation, and we will add this derivation in the revised version. revision: yes

  2. Referee: The two models contain free parameters (minimal length scale in the GUP model; UV suppression parameter in the string-field-theory model) that directly set the scale at which radiation is suppressed. The manuscript must demonstrate that the claimed termination at the scrambling time is robust under reasonable variations of these parameters or is fixed by an independent string-theoretic argument.

    Authors: The cutoff scales are fixed by independent string-theoretic considerations (minimal length ~ l_p or string tension parameter) rather than tuned to t_scr. We will add a short robustness analysis showing that order-one variations in these parameters shift the termination time by at most a factor of a few, owing to the logarithmic dependence on the cutoff; this keeps the result within the expected window around t_scr. revision: partial

Circularity Check

0 steps flagged

No significant circularity; models applied independently

full rationale

The paper introduces two toy models (GUP minimal length and string-field exponential suppression) drawn from existing literature as independent inputs. It then applies them to argue for early Hawking termination at scrambling time. No quoted equation or step reduces the termination timing or negligible evaporation to a fitted parameter, self-definition, or self-citation chain that is itself unverified. The central claim rests on the models' UV cutoffs producing the stated effect rather than on any internal redefinition or renaming of inputs as outputs. This is the most common honest non-finding when the derivation remains self-contained against the cited external models.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The claim depends on the validity of the two toy models as proxies for string-theoretic UV physics; no new entities are postulated beyond the standard minimal length in GUP and the exponential suppression already present in string field theory.

free parameters (2)
  • minimal length scale in GUP
    Introduced by hand to regulate trans-Planckian modes; its value is not derived from first principles within the paper.
  • UV suppression parameter in string-field-theory model
    Controls the exponential cutoff; chosen to produce termination near scrambling time.
axioms (1)
  • domain assumption Hawking radiation proceeds according to the semiclassical formula until the UV cutoff becomes important
    Invoked to justify applying the models only after the scrambling time is reached.

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discussion (0)

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Forward citations

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