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Copyright © 2020 Elsevier B.V. or its licensors or contributors.
We find that the end state of Hawking evaporation leads to black hole remnant, which could help to ameliorate the information paradox. We found that the effective emission surface can be either proportional to the square of the effective AdS length scale, or corresponds to the square of the impact parameter of the null geodesic that falls onto the photon orbit of the black hole.
However, such quantum black holes would instantly evaporate, either totally or leaving only a very weakly interacting residue. We prove that these remnants only exist in anti-de Sitter spacetime. 0000012100 00000 n
10-year back file (where available). [citation needed]. 35 225003. Export citation and abstract 0000010055 00000 n
A. Gravitation Theory and Gravitational Collapse, Chicago: University of Chicago Press, 1965 pages 80–81, This page was last edited on 23 September 2020, at 21:14. Please choose one of the options below.
You will only need to do this once. While there exist various candidates, the nature of dark matter remains unresolved.
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Minimum mass of a black hole. In this letter we study the process of Hawking radiation of a black hole assuming the existence of a limiting physical curvature scale.
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We use cookies to help provide and enhance our service and tailor content and ads. We show that such a constraint is not so fine-tuned. 0000109497 00000 n
In principle, a black hole can have any mass equal to or above about 2.2 × 10 −8 kg or 22 micrograms (the Planck mass). Find out more about journal subscriptions at your site. 0000029054 00000 n
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Nevertheless, we speculate on their possible relevance to our Universe as dark matter candidate, in view of the possibility that our Universe could be inherently anti-de Sitter-like, with a transient accelerated expansion phase. 0000006188 00000 n
In higher-dimensional spacetime, the strength of gravity increases more rapidly with decreasing distance than in three dimensions.
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If a sufficient amount of small black holes can be produced in the early universe, then the resultant BHRs can be an interesting candidate for DM.
Here we argue the contrary, that the generalized uncertainty principle may prevent their total evaporation in exactly the same way that the uncertainty principle prevents the hydrogen atom from.
On the other hand, a Schwarzschild black hole in asymptotic anti-de Sitter space would tunnel into the thermal soliton solution known as … We address the objections to the existence of white-hole remnants, discuss their stability, and show how the notions of entropy relevant in this context allow them to evade several no-go arguments. In this paper we briefly review these arguments, and discuss the reheating temperature as, While there exist various candidates, the identification of dark matter remains unresolved.
Computer simulations suggest that the probability of formation of a primordial black hole is inversely proportional to its mass. 0000006754 00000 n
Thus, a thermodynamic description breaks down.
For corporate researchers we can also follow up directly with your R&D manager, or the information
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We then investigate non-perturbative quantum gravity effects on the thermodynamics of Culetu black hole up to leading-order terms. If this is indeed the case and if a sufficient amount of small black holes can be produced in the early universe, then the resultant BHRs can be an interesting candidate for DM. The remnant solution of the paradox has long been viewed with suspicion, mostly because remnants seemed to be such exotic objects. 0000007186 00000 n
We briefly comment on the black hole information loss problem and the production of such black holes in collider experiments. All rights reserved. RIS. The remnant solution of the paradox has long been viewed with suspicion, mostly because remnants seemed to be such exotic objects.
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Even so, at that time, the Universe was not able to collapse into a singularity due to its uniform mass distribution and rapid growth. 0000018305 00000 n
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In this work we investigate a black hole solution in massive gravity with a degenerate fiducial metric often used in the literature. We find that such black holes radiate eternally and never completely evaporate. 0000077502 00000 n
Most famously, black holes were predicted by Einstein's theory of general relativity, which showed that when a massive star dies, it leaves behind a small, dense remnant core.
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", "The end of the world at the Large Hadron Collider? BibTeX
Nevertheless, we speculate on their possible relevance to our Universe as dark matter candidate, in view of the possibility that our Universe could be inherently anti-de Sitter-like, with a transient accelerated expansion phase. According to the formulae of black hole thermodynamics, the more the black hole loses mass, the hotter it becomes, and the faster it evaporates, until it approaches the Planck mass.
It has, however, been suggested that a small black hole of sufficient mass passing through the Earth would produce a detectable acoustic or seismic signal.[18][19][20][a].
They might be observed by astrophysicists through the particles they are expected to emit by Hawking radiation.
To read the article of this research, you can request a copy directly from the authors. Furthermore, depending on the black hole parameters, the emission surface could switch from one to another as the black hole loses mass during the evaporation process. The remnant of entropy is given by (22) S r = π Λ 2 γ 2 − (1 + ε) Λ − γ 2.. We present our results in Fig. 0000005669 00000 n
At this point then, the object can no longer be described as a classical black hole, and Hawking's calculations also break down.
The black hole has about 3.8 times the mass of our sun, and … Thus, the most likely outcome would be micro black holes. By assuming BHR as DM, our notion imposes a constraint on the, There have been proposals that primordial black hole remnants (BHRs) are the dark matter, but the idea is somewhat vague. Form and we will follow up with your librarian or Institution on your behalf. We then discuss in detail the existence and stability of remnants. In familiar three-dimensional gravity, the minimum energy of a microscopic black hole is 1019 GeV (equivalent to 1.6 GJ or 444 kWh), which would have to be condensed into a region on the order of the Planck length. Some hypotheses involving additional space dimensions predict that micro black holes could be formed at energies as low as the TeV range, which are available in particle accelerators such as the Large Hadron Collider.
At this stage, a black hole would have a Hawking temperature of TP/8π (5.6×1032 K), which means an emitted Hawking particle would have an energy comparable to the mass of the black hole.
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Published 19 October 2018, Method: Single-blind
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