Gravitational singularity

Lensing by a black hole. Animated simulation of gravitational lensing caused by a Schwarzschild black hole going past a background galaxy.

A gravitational singularity or spacetime singularity is a location where the quantities that are used to measure the gravitational field of a celestial body become infinite in a way that does not depend on the coordinate system. These quantities are the scalar invariant curvatures of spacetime, which includes a measure of the density of matter. The laws of normal spacetime could not exist within a singularity.[1][2]

For the purposes of proving the Penrose–Hawking singularity theorems, a spacetime with a singularity is defined to be one that contains geodesics that cannot be extended in a smooth manner.[3] The end of such a geodesic is considered to be the singularity. This is a different definition, useful for proving theorems.

The two most important types of spacetime singularities are curvature singularities and conical singularities.[4] Singularities can also be divided according to whether or not they are covered by an event horizon (naked singularities are not covered).[5] According to modern general relativity, the initial state of the universe, at the beginning of the Big Bang, was a singularity.[6] Both general relativity and quantum mechanics break down in describing the earliest moments of the Big Bang,[7] but in general, quantum mechanics does not permit particles to inhabit a space smaller than their wavelengths.[8] Another type of singularity predicted by general relativity is inside a black hole: any star collapsing beyond a certain point (the Schwarzschild radius) would form a black hole, inside which a singularity (covered by an event horizon) would be formed, as all the matter would flow into a certain point (or a circular line, if the black hole is rotating).[9] This is again according to general relativity without quantum mechanics, which forbids wavelike particles entering a space smaller than their wavelength. These hypothetical singularities are also known as curvature singularities.

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, renormalization, and instability of a hydrogen atom predicted by the Larmor formula.

In supersymmetry, a singularity in the moduli space happens usually when there are additional massless degrees of freedom in that certain point. Similarly, it is thought that singularities in spacetime often mean that there are additional degrees of freedom that exist only within the vicinity of the singularity. The same fields related to the whole spacetime also exist; for example, the electromagnetic field. In known examples of string theory, the latter degrees of freedom are related to closed strings, while the degrees of freedom are "stuck" to the singularity and related either to open strings or to the twisted sector of an orbifold.

Some theories, such as the theory of loop quantum gravity suggest that singularities may not exist.[10] 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.

Types

Curvature

A simple illustration of a non-spinning Black hole and its singularity

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. In order 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. 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.[11]

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 space-time curvature.

Conical

A conical singularity occurs when there is a point where the limit of every diffeomorphism invariant quantity is finite, 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 if a suitable coordinate system is used.

An example of such a conical singularity is a cosmic string.[12]

Naked

Main article: 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 have its geodesics terminated, thus making the naked singularity look like a Black Hole.[13][14][15]

Entropy

Further information: Black hole, Hawking radiation and Entropy

Before Stephen Hawking came up with the concept of Hawking radiation, the question of black holes having entropy was avoided. However, this concept demonstrates that black holes can 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 suggests that black holes do not last forever, but rather "evaporate" slowly. Small black holes tend to be hotter whereas larger ones tend to be colder. All known black hole candidates are so large that their temperature is far below that of the cosmic background radiation, so they are all gaining energy. They will not begin to lose energy until a cosmological redshift of more than one million is reached, rather than the thousand or so since the background radiation formed.

See also

Notes

  1. ↑ "Blackholes and Wormholes".
  2. ↑ "Spacetime Singularities".
  3. ↑ Moulay, Emmanuel. "The universe and photons" (PDF). FQXi Foundational Questions Institute. Retrieved 26 December 2012.
  4. ↑ Uggla, Claes. "Spacetime singularities". Einstein Online. Max Planck Institute for Gravitational Physics.
  5. ↑ Patrick Di Justo; Kevin Grazier; Patrick Grazier & Kevin Grazier (2010). The Science of Battlestar Galactica. New York: John Wiley & Sons. p. 181. ISBN 978-0470399095.
  6. ↑ Wald, p. 99
  7. ↑ Hawking, Stephen. "The Beginning of Time". Stephen Hawking: The Official Website. Cambridge University. Retrieved 26 December 2012.
  8. ↑ Zebrowski, Ernest (2000). A History of the Circle: Mathematical Reasoning and the Physical Universe. Piscataway NJ: Rutgers University Press. p. 180. ISBN 978-0813528984.
  9. ↑ Curiel, Erik & Peter Bokulich. "Singularities and Black Holes". Stanford Encyclopedia of Philosophy. Center for the Study of Language and Information, Stanford University. Retrieved 26 December 2012.
  10. ↑ Rodolfo Gambini, Javier Olmedo, Jorge Pullin. "Quantum black holes in Loop Quantum Gravity".
  11. ↑ 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.
  12. ↑ Copeland, Edmund J; Myers, Robert C; Polchinski, Joseph (2004). "Cosmic F- and D-strings". Journal of High Energy Physics 2004 (6): 013. arXiv:hep-th/0312067. Bibcode:2004JHEP...06..013C. doi:10.1088/1126-6708/2004/06/013.
  13. ↑ M. Bojowald. "Living Rev. Rel. 8, (2005), 11".
  14. ↑ R. Goswami & P. Joshi. "Phys. Rev. D, (2008)".
  15. ↑ R. Goswami, P. Joshi, & P. Singh. "Phys. Rev. Letters, (2006), 96".

References

Further reading

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