bcrowell said:
There have been a ton of exotic objects proposed that would be more compact than neutron stars but that would not be black holes. These include black stars, gravastars, fuzzballs, quark stars, boson stars, and q-balls.
I've seen some exotic proposals for "denser than neutron" matter. But do any of these "exotic matter" equations of state allow dense enough material to actually push the critical mass beyond that of the super massive black holes at the center of galaxies?
bcrowell said:
If you take semiclassical gravity seriously, then there's considerable doubt about whether black holes actually form; there was an article about this in Scientific American, Oct. 2009, by Carlos Barcelo, Stefano Liberati, Sebastiano Sonego, and Matt Visser.
I think I remember reading that. If it is the paper I remember, I thought the authors made it very clear this would not prevent all black holes. It was in essence a "dark star" solution ... a proposal for a quantum back reaction that could infinitely delay collapse of some black holes (essentially give a different equation of state density limit once including this back reaction).
Even if I'm unfortunately remembering another paper, the conventional take was that you should always be able to scale up a black hole to make it "classical" regardless of the quantum effects. An event horizon is only a global entity. For a quantum effect to break all black holes, it would somehow need to violate Lorentz symmetry on these huge scales ... for a free falling observer (in falling with dust which in the far future would become a singularity) could know about the pending event horizon from local measurements.
I remember reading a paper once about black holes in DeSitter spacetime which claimed there could be some strange issues. I don't remember the details. I know that is vague, but by any chance do you remember that discussion?
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EDIT:
The "Dark star" Scientific American paper doesn't appear to be freely available now. The "teaser" they give sounds like what I remember, but I found the paper the SA article is most likely based on, and they makes claims differently than I remember (I probably just remembered wrong, or maybe they toned down some claims for the SA article).
Fate of gravitational collapse in semiclassical gravity
Author(s): Barcelo C (Barcelo, Carlos)1, Liberati S (Liberati, Stefano)2,3, Sonego S (Sonego, Sebastiano)4, Visser M (Visser, Matt)5
Source: PHYSICAL REVIEW D Volume: 77 Issue: 4 Article Number: 044032 Published: FEB 2008
There is a free arxiv copy on the same subject by those authors here:
http://arxiv.org/abs/0902.0346
They mention the equivalence principle, and say it is implicitly held. I don't see their point of view here. It seems their proposal strongly violates the equivalence principle, since they claim the effects don't go away even if the size of the "would be" black hole is scaled up. This seems very suspect for reasons already mentioned.
Their paper was cited by:
"Radiation from collapsing shells, semiclassical backreaction, and black hole formation"
Author(s): Paranjape A (Paranjape, Aseem)1, Padmanabhan T (Padmanabhan, T.)2
Source: PHYSICAL REVIEW D Volume: 80 Issue: 4 Article Number: 044011 Published: AUG 2009
Abstract: We provide a detailed analysis of quantum field theory around a collapsing shell and discuss several conceptual issues related to the emission of radiation flux and formation of black holes. Explicit calculations are performed using a model for a collapsing shell, which turns out to be analytically solvable. We use the insights gained in this model to draw reliable conclusions regarding more realistic models. We first show that any shell of mass M, which collapses to a radius close to r=2M, will emit approximately thermal radiation for a period of time. In particular, a shell that collapses from some initial radius to a final radius 2M(1-epsilon(2))(-1) (where epsilon < 1) without forming a black hole, will emit thermal radiation during the period M less than or similar to t less than or similar to Mln(1/epsilon(2)). Later on (tMln(1/epsilon(2))), the flux from such a shell will decay to zero exponentially. We next study the effect of backreaction computed using the vacuum expectation value of the stress tensor on the collapse. We find that, in any realistic collapse scenario,
the backreaction effects do not prevent the formation of the event horizon. The time at which the event horizon is formed is, of course, delayed due to the radiated flux-which decreases the mass of the shell-but this effect is not sufficient to prevent horizon formation. We also clarify several conceptual issues and provide pedagogical details of the calculations in the Appendices to the paper.