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eternal black holes

Start here for a quick overview of the site The field equations without denominators in the case when In order to eliminate singularities, if one replaces The solution is free from singularities for all finite points in the space of the two sheets"Einstein-Rosen Bridge" redirects here. We didn't use $x<0$ for the outside, so let's use it. And if you are outside you can slope left (the most you can slope is 45 degrees to the left as you go up) and cross the event horizon.So that's a black hole that never formed but was just always there, the event horizon marks the inside versus the outside, once in you never escape and inside there is a singularity that can't be avoided once you cross in. This leads to some strange consequences (white holes, Einstein-Rosen bridges, ...) so one must be a little careful when interpreting the physics from these models.how could u form a black hole from nothing collapsing then?Albert, the eternal black hole is a non-physical solution; it is the Apologies for my ignorance, but how could we say that from the point of view of the observer that the black hole could exist forever, when the observer witnessed (and acknowledged) both the creation and the subsequent time before its creation?It's an idealized situation so from the point of view of the faraway observer they never witness any time before the creation of the black hole, even though this is not a realistic way to describe an actual black hole.So the observer only witnesses the hole's formation, and nothing else?No they never witness the formation of the black hole as from their point of view it is eternal (without temporal beginning or end).ah so an eternal black hole is just an idealization?I'll try to find a diagram to complement yours that shows qualitatively the (spherically symmetric) collapsing surface of a star. They're giant bundles of extremely dense matter. Set the line $y=x$ for $x>0$ to be the event horizon. Physics Stack Exchange works best with JavaScript enabled

Note that the event horizon looks like a surface of $t=+\infty$ and that's not an accident, that's because the time is time measured by the outside, and time on the outside never sees you cross, and never seeing is like seeing something that happened at $t=+\infty$ so you can see it get close to happening but you literally never see it happen.

For a normal (nonrotating) black hole, the hypotehtical singularity might fill the whole inside in such a way that if you cross the event horizon you will hit the singularity no matter what, it's in your future and in the way and every direction you take to the future after crossing the event horizon hit it.let's draw this.

An event horizon is a boundary from one region of spacetime and another such that you can only cross one way. But is there another way in beside coming from on of these black holes?Again, the math of GR allows yet another option. it is unavoidable, because we set up our metric to require the $y$ always get larger, and that you can angle at most 45 degrees (either right or left).So basically when $y>|x|$ you are inside the black hole.

So the Schwarzschild metric is only an approximate description of real black holes, though we would expect the approximation to be exceedingly good for a black hole of any reasonable age.Anyhow, the Schwarzschild metric is written using the Schwarzschild coordinates time $t$, radial distance $r$, and the angles $\theta$ and $\phi$. From the point of view of each of these regions the other region is behind the horizon. A point in the outside has already been fully affected by every part of the white hole and trying to move to the inside takes you to the black hole instead of the white hole. Just as the outside can treat the inside of the black hole as beyond the $t=+\infty$ surface since they can never see it.

A. Wheeler, "Causality and Multiply-Connected Space-Time," It's like the cemetary, you can go there, but you aren't going to talk to someone that is gone because they just aren't there anymore.That's the point of assigning coordinates to these event, so we can see what can affect what and take into account that rulers and clocks one person uses might be relative and different than what someone somewhere or somewhen else would expect.So the white hole can effect both outsides and the black hole, and either outside can get to the inside of the black hole but then will never get out. But the trouble is that the Schwarzschild coordinates are singular at the event horizon and badly behaved inside it ($r$ becomes timelike and $t$ spacelike).

It may just mean we've pushed the model beyond the bounds of its physical applicability. White holes appear in the theory of eternal black holes.

Region 3 is a region of spacetime outside the event horizon and linked to our patch of spacetime by a non-traversible wormhole (specifically an Einstein Rosen bridge). And we can set up the metric so that particles can go upwards always, and sloping towards the left is going into the black hole and sloping right (as you go up) is away.So once you cross the line $y=x$ even if you slope as far right as you can (45 degrees slope is moving at the speed of light away from the center) then you hit the singularity. It only takes a minute to sign up.Real black holes form through stellar collapse (and possibly a few other mechanisms) and from the point of view of an observer observing the black hole from a safe distance away they would be able to easily talk about a time before the black hole existed.When the first black hole solutions were created they used the idealization that black holes, from the point of the faraway observer, had always existed. But there are future pointing curves that go from outside to inside the event horizon.So we have spacetime, event horizons, and a black-hole singularity that lives inside. For something that contains so much emptiness, the universe is surprisingly full. By using our site, you acknowledge that you have read and understand our Physics Stack Exchange is a question and answer site for active researchers, academics and students of physics. For the EP by Venetian Snares, see Other computer-rendered images and animations of traversable wormholes can be seen on A. Einstein and N. Rosen, "The Particle Problem in the General Theory of Relativity," R. W. Fuller and J.

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