Line 18a3s2 No-Hair Theorem Black Hole Four-Dimension Event Horizon Redshift WOW SETI

Line 18a3s2  No-Hair Theorem Black Hole Four-Dimension Event Horizon Redshift WOW SETI

part 123 of 100 videos there are more videos after this one i’ll post all then update the #.
Math Equation Wow Seti 1977 radio signal alien

14/

3/4/4/1/1/1/1/11=0.017
14/0.017=823.5294

Feb 13 2012 911 pm est

My Thoughts

Were getting a lot of data about Black Holes, Speed, Velocity and measurements of the Universe showing up in the data.

I don’t quite understand any of it at this point. I hope I will as we go along…

Key word that shows up alot in the last three sections of data

Minkowski spacetime

High Energy Physics – Theory
Entanglement Interpretation of Black Hole Entropy in String Theory
Ram Brustein, Martin B. Einhorn, Amos Yarom
(Submitted on 29 Aug 2005)

1983 Wave function of the universe
Hawking has spent much of his time trying to develop a quantum theory of gravity. He started out applying his idea of Euclidean quantum gravity to black holes, but in 1983 teamed up with Jim Hartle at Chicago University. Together they proposed a “wave function of the universe” that, in theory, could be used to calculate the properties of the universe we see around us.

notes

quotes

The no-hair theorem postulates that all black hole solutions of the Einstein-Maxwell equations of gravitation and electromagnetism in general relativity can be completely characterized by only three externally observable classical parameters: mass, electric charge, and angular momentum.

All other information (for which “hair” is a metaphor) about the matter which formed a black hole or is falling into it, “disappears” behind the black-hole event horizon and is therefore permanently inaccessible to external observers.

It is considered a theorem by physicists. There is still no rigorous mathematical proof of the no-hair theorem, and mathematicians refer to it as the no-hair conjecture.

Four-dimensional space-time
The no-hair theorem was originally formulated for black holes within the context of a four-dimensional spacetime, obeying the Einstein field equation of general relativity with zero cosmological constant, in the presence of electromagnetic fields, or optionally other fields such as scalar fields and massive vector fields (Proca fields, spinor fields, etc.).[1]

Extensions
It has since been extended to include the case where the cosmological constant is positive (which recent observations are tending to support).[2]
Magnetic charge, if detected as predicted by some theories, would form the fourth parameter possessed by a classical black hole.

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inside the Event Horizon space is being pulled faster than the speed of light diagram wow seti

quote

Event Horizon 

In general relativity, an event horizon is a boundary in spacetime beyond which events cannot affect an outside observer.

In layman’s terms it is defined as “the point of no return” i.e.

the point at which the gravitational pull becomes so great as to make escape impossible. The most common case of an event horizon is that surrounding a black hole.

Light emitted from beyond the horizon can never reach the observer.

Likewise, any object approaching the horizon from the observer’s side appears to slow down and never quite pass through the horizon, with its image becoming more and more redshifted as time elapses.

The traveling object, however, experiences no strange effects and does, in fact, pass through the horizon in a finite amount of proper time.

More specific types of horizon include the related but distinct absolute and apparent horizons found around a black hole. Still other distinct notions include the Cauchy and Killing horizon; the photon spheres and ergospheres of the Kerr solution; particle and cosmological horizons relevant tocosmology; and isolated and dynamical horizons important in current black hole research.

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Absorption lines in the optical spectrum of a supercluster of distant galaxies (right), as compared to absorption lines in the optical spectrum of the Sun

Absorption lines in the optical spectrum of a supercluster of distant galaxies (right), as compared to absorption lines in the optical spectrum of the Sun (left). Arrows indicate redshift. Wavelength increases up towards the red and beyond (frequency decreases).

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1983 Wave function of the universe stephen hawking and james hartle big bang theory wow seti

1983 Wave function of the universe
Hawking has spent much of his time trying to develop a quantum theory of gravity. He started out applying his idea of Euclidean quantum gravity to black holes, but in 1983 teamed up with Jim Hartle at Chicago University. Together they proposed a “wave function of the universe” that, in theory, could be used to calculate the properties of the universe we see around us.

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quote

In 1981, Stephen Hawking and James Hartle came up with an imaginative proposal which promised to avoid the singularity at the origin of the universe, and also gave a answer to the question of why there was no time before the Big Bang. But before we can consider the theory, we need to introduce a couple of concepts.

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the hartle hawking no boundary expanding universe proposal euclidean region lorentzian region wow seti

Camera cut out here *** to be filmed with Line18a3s3 Kerr Black White Holes GRB 060614 Portals Time Travel WOW SETI
Feb 13 2012 11 29 pm est