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However, after Einstein, we knew that Newtonian mechanics must be wrong. At the very basic level, this theory is not correct because it is a scheme that works faster than the speed of light essentially, it claims that if you remove the Sun from our solar system, all the planets would begin spinning off into interstellar space before the last light of the Sun reached them i.

Einstein showed us how this theory is flawed through his explanation of the curvature of spacetime. But Einstein, just having written down the celebrated Einstein Field Equations describing the curvature of spacetime, began to fret.

Regardless, in essence, a black hole is something that pulls, and in stricter terms, it pulls from a place you do not want to get near.

In short, the Event Horizon of a black hole is a name we give to the region of spacetime beyond which anything that drops into it can never come back out.

Not even light itself. This is the reverse: A white hole spits out everything and nothing goes in. So while a black hole has an event horizon that, once you get close enough, you can never escape, a white hole has an event horizon that you can never even get close to and that is not even counting the burning that you would get when you try!

Share to Facebook. Tweet This. Here, "maximally extended" refers to the idea that the spacetime should not have any "edges": for any possible trajectory of a free-falling particle following a geodesic in the spacetime, it should be possible to continue this path arbitrarily far into the particle's future, unless the trajectory hits a gravitational singularity like the one at the center of the black hole's interior.

In order to satisfy this requirement, it turns out that in addition to the black hole interior region which particles enter when they fall through the event horizon from the outside, there must be a separate white hole interior region, which allows us to extrapolate the trajectories of particles which an outside observer sees rising up away from the event horizon.

For an observer outside using Schwarzschild coordinates , infalling particles take an infinite time to reach the black hole horizon infinitely far in the future, while outgoing particles which pass the observer have been traveling outward for an infinite time since crossing the white hole horizon infinitely far in the past however, the particles or other objects experience only a finite proper time between crossing the horizon and passing the outside observer.

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 which uses Kruskal—Szekeres coordinates see figure. In this spacetime, it is possible to come up with coordinate systems such that if you pick a hypersurface of constant time a set of points that all have the same time coordinate, such that every point on the surface has a space-like separation, giving what is called a 'space-like surface' and draw an "embedding diagram" 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" or Schwarzschild wormhole.

It is impossible to use the bridge to cross from one universe to the other, however, because it is impossible to enter a white hole event horizon from the outside, and anyone entering a black hole horizon from either universe will inevitably hit the black hole singularity.

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.

The time-reversed case would be a white hole that has existed since the beginning of the universe, and which emits matter until it finally "explodes" and disappears.

A view of black holes first proposed in the late s might be interpreted as shedding some light on the nature of classical white holes.

The Einstein—Cartan-Sciama-Kibble theory of gravity extends general relativity by removing a constraint of the symmetry of the affine connection and regarding its antisymmetric part, the torsion tensor , as a dynamical variable.

Torsion naturally accounts for the quantum-mechanical, intrinsic angular momentum spin of matter. According to general relativity, the gravitational collapse of a sufficiently compact mass forms a singular black hole.

In the Einstein—Cartan theory, however, the minimal coupling between torsion and Dirac spinors generates a repulsive spin—spin interaction which is significant in fermionic matter at extremely high densities.

Such an interaction prevents the formation of a gravitational singularity. Instead, the collapsing matter on the other side of the event horizon reaches an enormous but finite density and rebounds, forming a regular Einstein—Rosen bridge.

For observers in the baby universe, the parent universe appears as the only white hole. Accordingly, the observable universe is the Einstein—Rosen interior of a black hole existing as one of possibly many inside a larger universe.

The Big Bang was a nonsingular Big Bounce at which the observable universe had a finite, minimum scale factor.

A paper argues that the Big Bang itself is a white hole. Thus, unlike black holes, white holes cannot be continuously observed; rather, their effects can be detected only around the event itself.

The paper even proposed identifying a new group of gamma-ray bursts with white holes. In , the idea of the Big Bang being produced by a supermassive white hole explosion was explored in the framework of a five dimensional vacuum by Madriz Aguilar, Moreno and Bellini.

From Wikipedia, the free encyclopedia. For other uses, see White hole disambiguation. Introduction History. Fundamental concepts. Principle of relativity Theory of relativity Frame of reference Inertial frame of reference Rest frame Center-of-momentum frame Equivalence principle Mass—energy equivalence Special relativity Doubly special relativity de Sitter invariant special relativity World line Riemannian geometry.

Equations Formalisms. Birkhoff's theorem Geroch's splitting theorem Goldberg—Sachs theorem Lovelock's theorem No-hair theorem Penrose—Hawking singularity theorems Positive energy theorem.

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White pole black holes

The invisible spherical boundary surrounding the core of a black hole that marks its point of no return is known as its event horizon.

Black holes that lose more mass than they gain are expected to shrink and ultimately vanish. However, Rovelli and his colleagues suggested that shrinking black holes could not disappear if the fabric of space and time were quantum — that is, made of indivisible quantities known as quanta.

Space-time is quantum in research that seeks to unite general relativity, which can explain the nature of gravity, with quantum mechanics, which can describe the behavior of all the known particles, into a single theory that can explain all the forces of the universe.

In the study, Rovelli and his team suggested that, once a black hole evaporated to a degree where it could not shrink any further because space-time could not be squeezed into anything smaller, the dying black hole would then rebound to form a white hole.

Black holes nowadays are thought to form when massive stars die in giant explosions known as supernovas, which compress their corpses into the infinitely dense points known as singularities at the hearts of black holes.

Rovelli and his colleagues previously estimated that it would take a black hole with a mass equal to that of the sun about a quadrillion times the current age of the universe to convert into a white hole.

However, prior work in the s and s suggested that black holes also could have originated within a second after the Big Bang, due to random fluctuations of density in the hot, rapidly expanding newborn universe.

Areas where these fluctuations concentrated matter together could have collapsed to form black holes. Even white holes with microscopic diameters could still be quite massive, just as black holes smaller than a sand grain can weigh more than the moon.

Now, Rovelli and study co-author Francesca Vidotto, of the University of the Basque Country in Spain, suggest that these microscopic white holes could make up dark matter.

As its name suggests, dark matter is invisible; it does not emit, reflect or even block light. As a result, dark matter can currently be tracked only through its gravitational effects on normal matter, such as that making up stars and galaxies.

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Messier 87 galaxy — home of the first imaged black hole. See also: Accretion disk. See also: X-ray binary. Main article: Quasi-periodic oscillations.

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Main article: Black hole information paradox. Is physical information lost in black holes? In higher dimensions more complicated horizon topologies like a black ring are possible.

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1 Comments

  1. Akinogis Zologore

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