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. A wormhole (: Einstein–Rosen bridge) is a concept that represents a: a non-trivial structure linking separate points in. A wormhole can be visualized as a tunnel with two ends, each at separate points in spacetime (i.e., different locations and/or different points of time). Wormholes are consistent with the, but whether wormholes actually exist remains to be seen. A wormhole could connect extremely long distances such as a billion or more, short distances such as a few, different, or different points in time. Wormhole visualized For a simplified notion of a wormhole, can be visualized as a two-dimensional (2D) surface. In this case, a wormhole would appear as a hole in that surface, lead into a tube (the inside surface of a ), then re-emerge at another location on the 2D surface with a hole similar to the entrance.
An actual wormhole would be analogous to this, but with the spatial dimensions raised by one. For example, instead of circular holes on a, the entry and exit points could be visualized as spheres in.
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Another way to imagine wormholes is to take a sheet of paper and draw two somewhat distant points on one side of the paper. The sheet of paper represents a plane in the, and the two points represent a distance to be traveled, however theoretically a wormhole could connect these two points by folding that plane so the points are touching. In this way it would be much easier to traverse the distance since the two points are now touching. Terminology In 1928, proposed a wormhole theory of matter in connection with mass analysis of energy; however, he did not use the term 'wormhole' (he spoke of 'one-dimensional tubes' instead). American (inspired by Weyl's work) coined the term 'wormhole' in a 1957 paper co-authored by: This analysis forces one to consider situations.
Where there is a net flux of lines of force, through what would call 'a ' of the multiply-connected space, and what physicists might perhaps be excused for more vividly terming a 'wormhole'. — Charles Misner and John Wheeler in Modern definitions Wormholes have been defined both. From a topological point of view, an intra-universe wormhole (a wormhole between two points in the same universe) is a region of spacetime whose boundary is topologically trivial, but whose interior is not. Formalizing this idea leads to definitions such as the following, taken from 's Lorentzian Wormholes (1996). If a contains a compact region Ω, and if the topology of Ω is of the form Ω R × Σ, where Σ is a three-manifold of the nontrivial topology, whose boundary has topology of the form ∂Σ S 2, and if, furthermore, the Σ are all spacelike, then the region Ω contains a quasipermanent intrauniverse wormhole.
Geometrically, wormholes can be described as regions of spacetime that constrain the incremental deformation of closed surfaces. For example, in Enrico Rodrigo's The Physics of Stargates, a wormhole is defined informally as: a region of spacetime containing a ' (the time evolution of a closed surface) that cannot be continuously deformed (shrunk) to a (the time evolution of a point). Development. 'Embedding diagram' of a Schwarzschild wormholes The equations of the theory of have valid solutions that contain wormholes. The first type of wormhole solution discovered was the Schwarzschild wormhole, which would be present in the describing an eternal black hole, but it was found that it would collapse too quickly for anything to cross from one end to the other. Wormholes that could be crossed in both directions, known as, would only be possible if with negative could be used to stabilize them.
An artist's impression of a wormhole from an observer's perspective, crossing the of a Schwarzschild wormhole that bridges two different universes. The observer originates from the right, and another universe becomes visible in the center of the wormhole's shadow once the horizon is crossed, the observer seeing light that has fallen into the interior region from the other universe; however, this other universe is unreachable in the case of a Schwarzschild wormhole, as the bridge always collapses before the observer has time to cross it, and everything that has fallen through the event horizon of either universe is inevitably crushed in the. Schwarzschild wormholes, also known as Einstein–Rosen bridges (named after and ), are connections between areas of space that can be modeled as to the, and that are now understood to be intrinsic parts of the version of the describing an eternal black hole with no charge and no rotation. Here, 'maximally extended' refers to the idea that the should not have any 'edges': it should be possible to continue this path arbitrarily far into the particle's future or past for any possible trajectory of a free-falling particle (following a in the spacetime).
In order to satisfy this requirement, it turns out that in addition to the black hole interior region that particles enter when they fall through the from the outside, there must be a separate interior region that allows us to extrapolate the trajectories of particles that an outside observer sees rising up away from the event horizon. And just as there are two separate interior regions of the maximally extended spacetime, there are also two separate exterior regions, sometimes called two different 'universes', with the second universe allowing us to extrapolate some possible particle trajectories in the two interior regions. This means that the interior black hole region can contain a mix of particles that fell in from either universe (and thus an observer who fell in from one universe might be able to see light that fell in from the other one), and likewise particles from the interior white hole region can escape into either universe.
All four regions can be seen in a spacetime diagram that uses. In this spacetime, it is possible to come up with such that if a of constant time (a set of points that all have the same time coordinate, such that every point on the surface has a separation, giving what is called a 'space-like surface') is picked and an 'embedding diagram' drawn depicting the curvature of space at that time, the embedding diagram will look like a tube connecting the two exterior regions, known as an 'Einstein–Rosen bridge'. Note that the Schwarzschild metric describes an idealized black hole that exists eternally from the perspective of external observers; a more realistic black hole that forms at some particular time from a collapsing star would require a different metric. When the infalling stellar matter is added to a diagram of a black hole's history, it removes the part of the diagram corresponding to the white hole interior region, along with the part of the diagram corresponding to the other universe.
The Einstein–Rosen bridge was discovered by in 1916, a few months after Schwarzschild published his solution, and was rediscovered by Albert Einstein and his colleague Nathan Rosen, who published their result in 1935. However, in 1962, and published a paper showing that this type of wormhole is unstable if it connects two parts of the same universe, and that it will pinch off too quickly for light (or any particle moving slower than light) that falls in from one exterior region to make it to the other exterior region.
According to general relativity, the of a sufficiently compact mass forms a singular Schwarzschild black hole. In the –Sciama–Kibble theory of gravity, however, it forms a regular Einstein–Rosen bridge. This theory extends general relativity by removing a constraint of the symmetry of the and regarding its antisymmetric part, the, as a dynamical variable. Torsion naturally accounts for the quantum-mechanical, intrinsic angular momentum of matter. The minimal coupling between torsion and generates a repulsive spin–spin interaction that is significant in fermionic matter at extremely high densities. Such an interaction prevents the formation of a gravitational singularity.
Instead, the collapsing matter reaches an enormous but finite density and rebounds, forming the other side of the bridge. Although Schwarzschild wormholes are not traversable in both directions, their existence inspired to imagine traversable wormholes created by holding the 'throat' of a Schwarzschild wormhole open with (material that has negative mass/energy).
Other non-traversable wormholes include Lorentzian wormholes (first proposed by John Archibald Wheeler in 1957), wormholes creating a in a general relativistic spacetime manifold depicted by a, and Euclidean wormholes (named after, a structure of ). Traversable wormholes This shows that allows the energy density in certain regions of space to be negative relative to the ordinary matter, and it has been shown theoretically that quantum field theory allows states where energy can be arbitrarily at a given point. Many physicists, such as, and others, therefore argue that such effects might make it possible to stabilize a traversable wormhole. Physicists have not found any natural process that would be predicted to form a wormhole naturally in the context of general relativity, although the hypothesis is sometimes used to suggest that tiny wormholes might appear and disappear spontaneously at the,: 494–496 and stable versions of such wormholes have been suggested as candidates. It has also been proposed that, if a tiny wormhole held open by a had appeared around the time of the, it could have been inflated to size.
Wormhole travel as envisioned by Les Bossinas for The impossibility of faster-than-light relative speed only applies locally. Wormholes might allow effective superluminal travel by ensuring that the speed of light is not exceeded locally at any time. While traveling through a wormhole, subluminal (slower-than-light) speeds are used.
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If two points are connected by a wormhole whose length is shorter than the distance between them outside the wormhole, the time taken to traverse it could be less than the time it would take a light beam to make the journey if it took a path through the space outside the wormhole. However, a light beam traveling through the wormhole would of course beat the traveler. Time travel.