Absolute horizon

In general relativity, an absolute horizon is a boundary in spacetime, defined with respect to the external universe, inside which events cannot affect an external observer. Light emitted inside the horizon can never reach the observer, and anything that passes through the horizon from the observer's side is never seen again by the observer. An absolute horizon is thought of as the boundary of a black hole.

In the context of black holes, the absolute horizon is almost exclusively referred to as an event horizon, though this is often used as a more general term for all types of horizons. The absolute horizon is just one type of horizon. For example, important distinctions must be made between absolute horizons and apparent horizons; the notion of a horizon in general relativity is subtle, and depends on fine distinctions.

Definition

An absolute horizon is only defined in an asymptotically flat spacetime – a spacetime which approaches flat space as one moves far away from any massive bodies. Examples of asymptotically flat spacetimes include Schwarzschild and Kerr black holes. The FRW universe – which is believed to be a good model for our universe – is generally not asymptotically flat. Nonetheless, we can think of an isolated object in an FRW universe as being nearly an isolated object in an asymptotically flat universe.

The particular feature of asymptotic flatness which is needed is a notion of "future null infinity". This is the set of points which are approached asymptotically by null rays (light rays, for example) which can escape to infinity. This is the technical meaning of "external universe". These points are only defined in an asymptotically flat universe. An absolute horizon is defined as the boundary of a region from which null rays cannot escape to future null infinity.[1][2][3]

Nature of the absolute horizon

The definition of an absolute horizon is sometimes referred to as teleological, meaning that it cannot be known where the absolute horizon is without knowing the entire evolution of the universe, including the future. This is both an advantage and a disadvantage. The advantage is that this notion of a horizon is very geometrical, and does not depend on the observer, unlike apparent horizons, for example. The disadvantage is that it requires the full history (all the way into the future) of the spacetime to be known. In the case of numerical relativity, where a spacetime is simply being evolved into the future, only a finite portion of the spacetime can be known.

See also

• Cauchy horizon
• Cosmological horizon
• Ergosphere
• Killing horizon
• Naked singularity
• Particle horizon
• Photon sphere
• Reissner–Nordström solution
• Schwarzschild metric

References

1. Hawking, S. W. & Ellis, G. F. R. (1975). The large scale structure of space-time. Cambridge University Press.
2. Wald, Robert M. (1984). General Relativity. Chicago: University of Chicago Press.
3. Thorne, Kip S.; Misner, Charles; Wheeler, John (1973). Gravitation. W. H. Freeman and Company.

Further reading

• Kip Thorne (1994). Black Holes and Time Warps. W. W. Norton. This is a popular book, aimed at the lay reader, containing good discussion of horizons and black holes.

External links