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A gravitational singularity, spacetime singularity or simply singularity is a theoretical condition in which gravity is predicted to be so intense that spacetime itself would break down catastrophically. As such, a singularity is by definition no longer part of the regular spacetime and cannot be determined by "where" or "when". Gravitational singularities exist at a junction between general relativity and quantum mechanics; therefore, the properties of the singularity cannot be described without an established theory of quantum gravity. Trying to find a complete and precise definition of singularities in the theory of general relativity, the current best theory of gravity, remains a difficult problem. A singularity in general relativity can be defined by the scalar invariant curvature becoming infinite or, better, by a geodesic being incomplete.

Gravitational singularities are mainly considered in the context of general relativity, where density would become infinite at the center of a black hole without corrections from quantum mechanics, and within astrophysics and cosmology as the earliest state of the universe during the Big Bang. Physicists have not reached a consensus about what actually happens at the extreme densities predicted by singularities (including at the start of the Big Bang).

General relativity predicts that any object collapsing beyond a certain point (for stars this is the Schwarzschild radius) would form a black hole, inside which a singularity (covered by an event horizon) would be formed. The Penrose–Hawking singularity theorems define a singularity to have geodesics that cannot be extended in a smooth manner. The termination of such a geodesic is considered to be the singularity.

Modern theory asserts that the initial state of the universe, at the beginning of the Big Bang, was a singularity. In this case, the universe did not collapse into a black hole, because currently-known calculations and density limits for gravitational collapse are usually based upon objects of relatively constant size, such as stars, and do not necessarily apply in the same way to rapidly expanding space such as the Big Bang. Neither general relativity nor quantum mechanics can currently describe the earliest moments of the Big Bang, but in general, quantum mechanics does not permit particles to inhabit a space smaller than their Compton wavelengths.

Interpretation

Many theories in physics have mathematical singularities of one kind or another. Equations for these physical theories predict that the ball of mass of some quantity becomes infinite or increases without limit. This is generally a sign for a missing piece in the theory, as in the ultraviolet catastrophe, re-normalization, and instability of a hydrogen atom predicted by the Larmor formula.

In classical field theories, including special relativity but not general relativity, one can say that a solution has a singularity at a particular point in spacetime where certain physical properties become ill-defined, with spacetime serving as a background field to locate the singularity. A singularity in general relativity, on the other hand, is more complex because spacetime itself becomes ill-defined, and the singularity is no longer part of the regular spacetime manifold. In general relativity, a singularity cannot be defined by "where" or "when".

Some theories, such as the theory of loop quantum gravity, suggest that singularities may not exist. This is also true for such classical unified field theories as the Einstein–Maxwell–Dirac equations. The idea can be stated in the form that, due to quantum gravity effects, there is a minimum distance beyond which the force of gravity no longer continues to increase as the distance between the masses becomes shorter, or alternatively that interpenetrating particle waves mask gravitational effects that would be felt at a distance.

Motivated by such philosophy of loop quantum gravity, recently it has been shown that such conceptions can be realized through some elementary constructions based on the refinement of the first axiom of geometry, namely, the concept of a point by considering Klein's prescription of accounting for the extension of a small spot that represents or demonstrates a point, which was a programmatic call that he called as a fusion of arithmetic and geometry. Klein's program, according to Born, was actually a mathematical route to consider 'natural uncertainty in all observations' while describing 'a physical situation' by means of 'real numbers'.

Types

There is only one type of singularity, each with different physical features that have characteristics relevant to the theories from which they originally emerged, such as the different shapes of the singularities, conical and curved. They have also been hypothesized to occur without event horizons, structures that delineate one spacetime section from another in which events cannot affect past the horizon; these are called naked.

Conical

A conical singularity occurs when there is a point where the limit of some diffeomorphism invariant quantity does not exist or is infinite, in which case spacetime is not smooth at the point of the limit itself. Thus, spacetime looks like a cone around this point, where the singularity is located at the tip of the cone. The metric can be finite everywhere the coordinate system is used.

An example of such a conical singularity is a cosmic string and a Schwarzschild black hole.

Curvature

Solutions to the equations of general relativity or another theory of gravity (such as supergravity) often result in encountering points where the metric blows up to infinity. However, many of these points are completely regular, and the infinities are merely a result of using an inappropriate coordinate system at this point. To test whether there is a singularity at a certain point, one must check whether at this point diffeomorphism invariant quantities (i.e. scalars) become infinite. Such quantities are the same in every coordinate system, so these infinities will not "go away" by a change of coordinates.

An example is the Schwarzschild solution that describes a non-rotating, uncharged black hole. In coordinate systems convenient for working in regions far away from the black hole, a part of the metric becomes infinite at the event horizon. However, spacetime at the event horizon is regular. The regularity becomes evident when changing to another coordinate system (such as the Kruskal coordinates), where the metric is perfectly smooth. On the other hand, in the center of the black hole, where the metric becomes infinite as well, the solutions suggest a singularity exists. The existence of the singularity can be verified by noting that the Kretschmann scalar, being the square of the Riemann tensor i.e. ${\displaystyle R_{\mu \nu \rho \sigma }R^{\mu \nu \rho \sigma }}$, which is diffeomorphism invariant, is infinite.

While in a non-rotating black hole the singularity occurs at a single point in the model coordinates, called a "point singularity", in a rotating black hole, also known as a Kerr black hole, the singularity occurs on a ring (a circular line), known as a "ring singularity". Such a singularity may also theoretically become a wormhole.

More generally, a spacetime is considered singular if it is geodesically incomplete, meaning that there are freely-falling particles whose motion cannot be determined beyond a finite time, being after the point of reaching the singularity. For example, any observer inside the event horizon of a non-rotating black hole would fall into its center within a finite period of time. The classical version of the Big Bang cosmological model of the universe contains a causal singularity at the start of time (t=0), where all time-like geodesics have no extensions into the past. Extrapolating backward to this hypothetical time 0 results in a universe with all spatial dimensions of size zero, infinite density, infinite temperature, and infinite spacetime curvature.

Naked singularity

Until the early 1990s, it was widely believed that general relativity hides every singularity behind an event horizon, making naked singularities impossible. This is referred to as the cosmic censorship hypothesis. However, in 1991, physicists Stuart Shapiro and Saul Teukolsky performed computer simulations of a rotating plane of dust that indicated that general relativity might allow for "naked" singularities. What these objects would actually look like in such a model is unknown. Nor is it known whether singularities would still arise if the simplifying assumptions used to make the simulation were removed. However, it is hypothesized that light entering a singularity would similarly have its geodesics terminated, thus making the naked singularity look like a black hole.

Disappearing event horizons exist in the Kerr metric, which is a spinning black hole in a vacuum, if the angular momentum (${\displaystyle J}$) is high enough. Transforming the Kerr metric to Boyer–Lindquist coordinates, it can be shown that the coordinate (which is not the radius) of the event horizon is, ${\displaystyle r_{\pm }=\mu \pm \left(\mu ^{2}-a^{2}\right)^{1/2}}$, where ${\displaystyle \mu =GM/c^{2}}$, and ${\displaystyle a=J/Mc}$. In this case, "event horizons disappear" means when the solutions are complex for ${\displaystyle r_{\pm }}$, or ${\displaystyle \mu ^{2}<a^{2}}$. However, this corresponds to a case where ${\displaystyle J}$ exceeds ${\displaystyle GM^{2}/c}$ (or in Planck units, ${\displaystyle J>M^{2}}$); i.e. the spin exceeds what is normally viewed as the upper limit of its physically possible values.

Similarly, disappearing event horizons can also be seen with the Reissner–Nordström geometry of a charged black hole if the charge (${\displaystyle Q}$) is high enough. In this metric, it can be shown that the singularities occur at ${\displaystyle r_{\pm }=\mu \pm \left(\mu ^{2}-q^{2}\right)^{1/2}}$, where ${\displaystyle \mu =GM/c^{2}}$, and ${\displaystyle q^{2}=GQ^{2}/\left(4\pi \epsilon _{0}c^{4}\right)}$. Of the three possible cases for the relative values of ${\displaystyle \mu }$ and ${\displaystyle q}$, the case where ${\displaystyle \mu ^{2}<q^{2}}$ causes both ${\displaystyle r_{\pm }}$ to be complex. This means the metric is regular for all positive values of ${\displaystyle r}$, or in other words, the singularity has no event horizon. However, this corresponds to a case where ${\displaystyle Q/{\sqrt {4\pi \epsilon _{0}}}}$ exceeds ${\displaystyle M{\sqrt {G}}}$ (or in Planck units, ${\displaystyle Q>M}$); i.e. the charge exceeds what is normally viewed as the upper limit of its physically possible values. Also, actual astrophysical black holes are not expected to possess any appreciable charge.

A black hole possessing the lowest ${\displaystyle M}$ value consistent with its ${\displaystyle J}$ and ${\displaystyle Q}$ values and the limits noted above; i.e., one just at the point of losing its event horizon, is termed extremal.

Entropy

Before Stephen Hawking came up with the concept of Hawking radiation, the question of black holes having entropy had been avoided. However, this concept demonstrates that black holes radiate energy, which conserves entropy and solves the incompatibility problems with the second law of thermodynamics. Entropy, however, implies heat and therefore temperature. The loss of energy also implies that black holes do not last forever, but rather evaporate or decay slowly. Black hole temperature is inversely related to mass. All known black hole candidates are so large that their temperature is far below that of the cosmic background radiation, which means they will gain energy on net by absorbing this radiation. They cannot begin to lose energy on net until the background temperature falls below their own temperature. This will occur at a cosmological redshift of more than one million, rather than the thousand or so since the background radiation formed.

See also

• 0-dimensional singularity: magnetic monopole
• 1-dimensional singularity: cosmic string
• 2-dimensional singularity: domain wall
• Fuzzball (string theory)
• Penrose–Hawking singularity theorems
• White hole
• BKL singularity
• Initial singularity

References

1. Earman 1995, pp. 28–31, Section 2.2 What is a singularity?
2. ^ Curiel, Erik (2021). "Singularities and Black Holes". Stanford Encyclopedia of Philosophy. Metaphysics Research Lab, Stanford University. Retrieved 1 October 2021.
3. "Singularities". Physics of the Universe.
4. Uggla, Claes (2006). "Spacetime Singularities". Einstein Online. 2 (1002). Max Planck Institute for Gravitational Physics. Archived from the original on 2017-01-24. Retrieved 2015-10-20.
5. Earman 1995, Chapter 8 "Afterword".
6. Moulay, Emmanuel. "The universe and photons" (PDF). FQXi Foundational Questions Institute. Retrieved 26 December 2012.
7. Wald 1984, p. 99.
8. Hawking, Stephen. "The Beginning of Time". Stephen Hawking: The Official Website. Cambridge University. Archived from the original on 6 October 2014. Retrieved 26 December 2012.
9. Zebrowski, Ernest (2000). A History of the Circle: Mathematical Reasoning and the Physical Universe. Piscataway New Jersey: Rutgers University Press. p. 180. ISBN 978-0813528984.
10. Ashtekar, Abhay (2005). "3: "The nature of spacetime singularities" by Alan D. Randall". In Ashtekar, Abhay (ed.). 100 years of relativity: space-time structure, Einstein and beyond. Singapore: World Scientific. ISBN 978-981-256-394-1.
11. Gambini, Rodolfo; Olmedo, Javier; Pullin, Jorge (2014-05-07). "Quantum black holes in loop quantum gravity". Classical and Quantum Gravity. 31 (9): 095009. arXiv:1310.5996. Bibcode:2014CQGra..31i5009G. doi:10.1088/0264-9381/31/9/095009. ISSN 0264-9381. S2CID 119247455.{{cite journal}}: CS1 maint: date and year (link)
12. Majhi, Abhishek (2022). "Resolving the Singularity by Looking at the Dot and Demonstrating the Undecidability of the Continuum Hypothesis". Foundations of Science. 29 (2): 405–440. doi:10.1007/s10699-022-09875-9. ISSN 1233-1821. S2CID 246942045.
13. Euclides; Heiberg, J. L.; Fitzpatrick, R. (2008). Fitzpatrick, Richard (ed.). Euclid's elements of geometry: the Greek text of J. L. Heiberg (1883–1885): from Euclidis Elementa, edidit et Latine interpretatus est I. L. Heiberg, in aedibus B. G. Teubneri, 1883–1885 (PDF). Translated by Fitzpatrick, Richard (Revised and corrected ed.). s.n. ISBN 978-0-615-17984-1.
14. Klein, Felix (2016). Elementary Mathematics From A Higher Standpoint. Springer Berlin Heidelberg. ISBN 978-3662495155.
15. Klein, Felix (2011). The Evanston Colloquium Lectures on Mathematics Delivered From August 28 to September 9, 1893 Before Members of the Congress of Mathematics Held in Connection with the World's Fair in Chicago, Illinois (PDF). The Project Gutenberg.
16. Born, Max (1968). Physics in My Generation. Springer New York.
17. Copeland, Edmund J.; Myers, Robert C.; Polchinski, Joseph (2004). "Cosmic F- and D-strings". Journal of High Energy Physics. 2004 (6): 13. arXiv:hep-th/0312067. Bibcode:2004JHEP...06..013C. doi:10.1088/1126-6708/2004/06/013. S2CID 140465.
18. If a rotating singularity is given a uniform electrical charge, a repellent force results, causing a ring singularity to form. The effect may be a stable wormhole, a non-point-like puncture in spacetime that may be connected to a second ring singularity on the other end. Although such wormholes are often suggested as routes for faster-than-light travel, such suggestions ignore the problem of escaping the black hole at the other end, or even of surviving the immense tidal forces in the tightly curved interior of the wormhole.
19. Bojowald, Martin (2008). "Loop Quantum Cosmology". Living Reviews in Relativity. 11 (1): 4. Bibcode:2008LRR....11....4B. doi:10.12942/lrr-2008-4. ISSN 2367-3613. PMC 5255532. PMID 28163606.
20. Goswami, Rituparno; Joshi, Pankaj S. (2008). "Spherical gravitational collapse in N dimensions". Physical Review D. 76 (8): 084026. arXiv:gr-qc/0608136. Bibcode:2007PhRvD..76h4026G. doi:10.1103/PhysRevD.76.084026. ISSN 1550-7998. S2CID 119441682.
21. Goswami, Rituparno; Joshi, Pankaj S.; Singh, Parampreet (2006-01-27). "Quantum Evaporation of a Naked Singularity". Physical Review Letters. 96 (3): 031302. arXiv:gr-qc/0506129. Bibcode:2006PhRvL..96c1302G. doi:10.1103/PhysRevLett.96.031302. ISSN 0031-9007. PMID 16486681. S2CID 19851285.{{cite journal}}: CS1 maint: date and year (link)
22. Hobson, Efstathiou & Lasenby 2013, pp. 300–305.
23. Hobson, Efstathiou & Lasenby 2013, pp. 320–325.
24. LoPresto, M. C. (2003). "Some Simple Black Hole Thermodynamics". The Physics Teacher. 41 (5): 299–301. Bibcode:2003PhTea..41..299L. doi:10.1119/1.1571268. S2CID 122758428.

Bibliography

• Earman, John (1995). Bangs, crunches, whimpers, and shrieks: Singularities and acausalities in relativistic spacetimes. Oxford University Press. ISBN 019509591X.
• Joshi, Pankaj S (2007). Gravitational collapse and spacetime singularities. New York: Cambridge University Press. ISBN 9781107405363.
• Misner, Charles W.; Thorne, Kip; Wheeler, John Archibald (1973). Gravitation. W. H. Freeman. ISBN 0-7167-0344-0. §31.2 The nonsingularity of the gravitational radius, and following sections; §34 Global Techniques, Horizons, and Singularity Theorems
• Wald, Robert M. (1984). General Relativity. University of Chicago Press. ISBN 0-226-87033-2.
• Hawking, S. W.; Penrose, R. (1970). "The singularities of gravitational collapse and cosmology". Proceedings of the Royal Society of London. A. Mathematical and Physical Sciences. 314 (1519): 529–548. Bibcode:1970RSPSA.314..529H. doi:10.1098/rspa.1970.0021. ISSN 0080-4630.
• Shapiro, Stuart L.; Teukolsky, Saul A. (1991). "Formation of naked singularities: The violation of cosmic censorship". Physical Review Letters. 66 (8): 994–997. Bibcode:1991PhRvL..66..994S. doi:10.1103/PhysRevLett.66.994. ISSN 0031-9007. PMID 10043968. S2CID 7830407.
• Penrose, Roger (December 1996). "Chandrasekhar, black holes, and singularities" (PDF). Journal of Astrophysics and Astronomy. 17 (3–4): 213–231. Bibcode:1996JApA...17..213P. doi:10.1007/BF02702305. ISSN 0250-6335.
• Penrose, Roger (December 1999). "The question of cosmic censorship" (PDF). Journal of Astrophysics and Astronomy. 20 (3–4): 233–248. Bibcode:1999JApA...20..233P. doi:10.1007/BF02702355. ISSN 0250-6335.
• Singh, T. P. (December 1999). "Gravitational collapse, black holes and naked singularities" (PDF). Journal of Astrophysics and Astronomy. 20 (3–4): 221–232. arXiv:gr-qc/9805066. Bibcode:1999JApA...20..221S. doi:10.1007/BF02702354. ISSN 0250-6335.
• Hobson, Michael P.; Efstathiou, George; Lasenby, Anthony (2013). General relativity: an introduction for physicists (1. publ., 6. print ed.). Cambridge: Cambridge University Press. ISBN 978-0-521-82951-9.

Further reading

• The Elegant Universe by Brian Greene. This book provides a layman's introduction to string theory, although some of the views expressed have already become outdated. His use of common terms and his providing of examples throughout the text help the layperson understand the basics of string theory.

v t e Relativity
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General relativity	Background Introduction Mathematical formulation Fundamental concepts Equivalence principle Riemannian geometry Penrose diagram Geodesics Mach's principle Formulation ADM formalism BSSN formalism Einstein field equations Linearized gravity Post-Newtonian formalism Raychaudhuri equation Hamilton–Jacobi–Einstein equation Ernst equation Phenomena Black hole Event horizon Singularity Two-body problem Gravitational waves: astronomy detectors (LIGO and collaboration Virgo LISA Pathfinder GEO) Hulse–Taylor binary Other tests: precession of Mercury lensing (together with Einstein cross and Einstein rings) redshift Shapiro delay frame-dragging / geodetic effect (Lense–Thirring precession) pulsar timing arrays Advanced theories Brans–Dicke theory Kaluza–Klein Quantum gravity Solutions Cosmological: Friedmann–Lemaître–Robertson–Walker (Friedmann equations) Lemaître–Tolman Kasner BKL singularity Gödel Milne Spherical: Schwarzschild (interior Tolman–Oppenheimer–Volkoff equation) Reissner–Nordström Axisymmetric: Kerr (Kerr–Newman) Weyl−Lewis−Papapetrou Taub–NUT van Stockum dust discs Others: pp-wave Ozsváth–Schücking Alcubierre In computational physics: Numerical relativity
Scientists	Poincaré Lorentz Einstein Hilbert Schwarzschild de Sitter Weyl Eddington Friedmann Lemaître Milne Robertson Chandrasekhar Zwicky Wheeler Choquet-Bruhat Kerr Zel'dovich Novikov Ehlers Geroch Penrose Hawking Taylor Hulse Bondi Misner Yau Thorne Weiss others
Category

v t e Black holes
Outline
Types	BTZ black hole Schwarzschild Rotating Charged Virtual Kugelblitz Supermassive Primordial Direct collapse Rogue Malament–Hogarth spacetime
Size	Micro Extremal Electron Stellar Microquasar Intermediate-mass Supermassive Active galactic nucleus Quasar LQG Blazar OVV
Formation	Stellar evolution Gravitational collapse Neutron star Related links Tolman–Oppenheimer–Volkoff limit White dwarf Related links Supernova Micronova Hypernova Related links Gamma-ray burst Binary black hole Quark star Supermassive star Quasi-star Supermassive dark star X-ray binary
Properties	Astrophysical jet Gravitational singularity Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Microlens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics Bekenstein bound Bousso's holographic bound Immirzi parameter Schwarzschild radius Spaghettification
Issues	Black hole complementarity Information paradox Cosmic censorship ER = EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem
Metrics	Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward
Alternatives	Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball Geon
Analogs	Optical black hole Sonic black hole
Lists	Black holes Most massive Nearest Quasars Microquasars
Related	Outline of black holes Black Hole Initiative Black hole starship Black holes in fiction Big Bang Big Bounce Compact star Exotic star Quark star Preon star Gravitational waves Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Population III star Supermassive star Quasi-star Supermassive dark star Rossi X-ray Timing Explorer Superluminal motion Timeline of black hole physics White hole Wormhole Tidal disruption event Planet Nine
Notable	Cygnus X-1 XTE J1650-500 XTE J1118+480 A0620-00 Sagittarius A* Centaurus A Phoenix Cluster PKS 1302-102 OJ 287 SDSS J0849+1114 TON 618 MS 0735.6+7421 NeVe 1 Hercules A 3C 273 Q0906+6930 Markarian 501 ULAS J1342+0928 PSO J030947.49+271757.31 AT2018hyz Swift J1644+57
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