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JesseM said:Hmm, I would have thought there wouldn't be a very close analogy to the classical case, since nothing new or unusual happens when you introduce point masses of infinite density into Newtonian physics or point charges of infinite charge density into electromagnetism, but singularities in GR are associated with phenomena that you don't see in extended non-collapsing masses, namely event horizons and the termination of worldlines which hit the singularities.
Basically, I was suggesting that to find out if there is a black hole, you look for a "trapped null surface" - a region from which light can't escape.
Without a trapped null surface, you have no event horizon (and hence no black hole).
Unfortunately, while the presence of a trapped null surface proves that there must be a singularity by Penrose's theorem, the absence of a trapped null surface doesn't actually prove that there isn't a singularity if you want to get reallly technical.
So my argument doesn't really rule out a singularity, but it does rule out a black hole.
Suppose we had a 2D spherical surface in GR whose radius was larger than than the Schwarzschild radius for that mass--would it still have an event horizon near the surface (if not, would it be a form of 'naked singularity'?) and would wordlines hitting it still be terminated? What does this mean in the case of an extended mass whose radius is larger than the Schwarzschild radius and whose pressure keeps it from collapsing, like a star? I assume it'd only be identical to the Schwarzschild solution beyond its surface, but not inside it?
You should be able to see that there isn't any trapped null surface for a sphere of mass M and radius R such that r is larger than the Schwarzschild radius of M.
The spherical symmetry of the problem guarantees that there will be a spherically symmetrical solution.
The 'r' coordinate can be defined as a radial coordinate where scaled such that the a circle of that radius has a circumference of 2*Pi*r, or alternately, an area of 4*Pi*r^2. (r is not a distance from the center, but is a function of distance from the center.)
Birkhoff's theorem says that the metric is going to be -(1-2M/r) dt^2 + 1/(1-2M/r) dr^2 for r > R, where 2*Pi*R is the circumference of the sphere.
The metric will be -(1 - 2M/R) dt^2 + 1/(1-2M/R) dr^2 for r<=R
This is essentially what George said earlier.
To calculate the curvature tensor for the above metric you do have to comit the minor sin of allowing delta functions, otherwise you have to insist that the sphere is really very thin, rather than having zero thickness.
You can see by inspection that for R > 2M the metric is well behaved - it's the same metric outside the sphere for anybody of mass M and radius r>R, basically. And inside the sphere, it's just a Minkowski metric.