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Black holes turn white fast, otherwise stay black: no half measures
General Relativity and Quantum Cosmology · Submitted 2 Nov 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We conclude that transitions with long characteristic time scales are pathologically unstable: occasional perturbations away from the perfect vacuum around these compact objects, even if being imperceptibly small, suffocate the white hole explosion.
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The abstract, sentence by sentence
Recently, various authors have proposed that the first ultraviolet effect on the gravitational collapse of massive stars to black holes is the transition between a black-hole geometry and a white-hole geometry, though their proposals are radically different in terms of their physical interpretation and characteristic time scales [1,2]. Several decades ago, it was shown by Eardley that white holes are highly unstable to the accretion of small amounts of matter, being rapidly turned into black holes [3]. Studying the crossing of null shells on geometries describing the black-hole to white-hole transition, we obtain the conditions for the instability to develop in terms of the parameters of these geometries. We conclude that transitions with long characteristic time scales are pathologically unstable: occasional perturbations away from the perfect vacuum around these compact objects, even if being imperceptibly small, suffocate the white hole explosion. On the other hand, geometries with short characteristic time scales are shown to be robust against perturbations, so that the corresponding processes could take place in real astrophysical scenarios. This motivates a conjecture about the transition amplitudes of different decay channels for black holes in a suitable ultraviolet completion of general relativity.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Recently, various authors have proposed that the first ultraviolet effect on the gravitational collapse of massive stars to black holes is the transition between a black-hole geometry and a white-hole geometry, though their proposals are radically different in terms of their physical interpretation and characteristic time scales [1,2]. | background 1.00 | 0.03 | 0.03 | asserted 0.49 |
| s1 | Several decades ago, it was shown by Eardley that white holes are highly unstable to the accretion of small amounts of matter, being rapidly turned into black holes [3]. | background 1.00 | 0.02 | 0.04 | asserted 1.00 |
| s2 | Studying the crossing of null shells on geometries describing the black-hole to white-hole transition, we obtain the conditions for the instability to develop in terms of the parameters of these geometries. | contribution 0.52 | 0.95 | 0.03 | asserted 0.99 |
| s3 | We conclude that transitions with long characteristic time scales are pathologically unstable: occasional perturbations away from the perfect vacuum around these compact objects, even if being imperceptibly small, suffocate the white hole explosion. | result 0.84 | 0.84 | 0.64 | asserted 1.00 |
| s4 | On the other hand, geometries with short characteristic time scales are shown to be robust against perturbations, so that the corresponding processes could take place in real astrophysical scenarios. | result 0.89 | 0.87 | 0.18 | hedged possibility 0.75 |
| s5 | This motivates a conjecture about the transition amplitudes of different decay channels for black holes in a suitable ultraviolet completion of general relativity. | interpretation 0.75 | 0.25 | 0.09 | speculative 0.92 |
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Original abstract
Recently, various authors have proposed that the first ultraviolet effect on the gravitational collapse of massive stars to black holes is the transition between a black-hole geometry and a white-hole geometry, though their proposals are radically different in terms of their physical interpretation and characteristic time scales [1,2]. Several decades ago, it was shown by Eardley that white holes are highly unstable to the accretion of small amounts of matter, being rapidly turned into black holes [3]. Studying the crossing of null shells on geometries describing the black-hole to white-hole transition, we obtain the conditions for the instability to develop in terms of the parameters of these geometries. We conclude that transitions with long characteristic time scales are pathologically unstable: occasional perturbations away from the perfect vacuum around these compact objects, even if being imperceptibly small, suffocate the white hole explosion. On the other hand, geometries with short characteristic time scales are shown to be robust against perturbations, so that the corresponding processes could take place in real astrophysical scenarios. This motivates a conjecture about the transition amplitudes of different decay channels for black holes in a suitable ultraviolet completion of general relativity.
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References
How the literature uses it
30 arXiv papers cite this in 49 sentences
Papers citing it · 37 sentences without a confident label
Compares with it 1 paper
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This repulsive effect resembles a quantum mechanical bounce discussed in the work by Barceló et al. [ref] and the references therein.
Stability of white holes revisited · Interaction of white hole with radial flows of matter · 0.96
Cites it as support 1 paper
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The point here is that gravitational interactions of the outgoing shell from the white hole with even a small amount of infalling matter (e.g., a photon from the cosmic microwave background) can cause the shell to recollapse into a new black hole [ref] .
The Black Hole information problem: past, present, and future · Sources of Drama · 0.98
Cites it as background 10 papers
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It is generally believed that the white holes, T-symmetrical analogs of the black holes, become unstable when they start interacting with external matter, see the papers by Eardley [ref] , Ori and Poisson [ref] , Barceló et al. [ref] .
Stability of white holes revisited · Introduction · 0.86
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In the absence of a fundamental quantum gravity theory which allows us to evaluate the dynamical evolution of matter collapse scenarios in a systematic manner, there has been a lot of work recently, highlighted by several authors, as to achieve such a scenario effectively [ref] .
Effective black-to-white hole bounces: The cost of surgery · Introduction · 0.91
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This paper considered Planck stars, objects also studied in [ref] and references therein.
RDM-stars as sources of fast radio bursts · Introduction · 0.81
What it cites · 10 sentences without a confident label
Cites as support 1 paper
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Our analysis singles out the geometries with short characteristic time scales [ref] as the only reasonable candidates to describe physical processes.
Where does the physics of extreme gravitational collapse reside? · Conclusions · 0.98
Cites as background 1 paper
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There is a large amount of literature considering the possible ultraviolet effects in the gravitational collapse of massive stars to black holes; see [ref] for a brief review and references therein.
Where does the physics of extreme gravitational collapse reside? · Introduction · 1.00
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