Timeline for Problems with fuzzball black hole creation and low energy physics
Current License: CC BY-SA 4.0
10 events
| when toggle format | what | by | license | comment | |
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| Feb 4 at 10:05 | history | bounty ended | Michael C. | ||
| Jan 28 at 23:35 | comment | added | Rexcirus | The complementarity argument seems to be very hand-wavy, but basically the quantum fuzzball could "oscillate" (as in quantum harmonic oscillations) in such a way to simulate the experience of a semi-classical behaviour, which would arise as hydrodynamic limit of the ensemble of fine-grained geometries. I've always seen this argument written for infalling observers, but it seems to me to be extendible to the inside too. Of course if the observer is very close to the would-be-singularity the situation would be quickly very dramatic, as if it were close to a black hole singularity. | |
| Jan 28 at 22:55 | vote | accept | Michael C. | ||
| Jan 28 at 22:55 | comment | added | Michael C. | Thank you. Right before you posted your reply, I just remembered how it's possible to reformulate an Oppenheimer-Snyder pressureless dust collapse into the collapse of an independent collection of concentric shells, which makes the transition between the 2 scenarios much easier to conceptualize. Can you elaborate on the "complementarity" you referred to which would seemingly still allow an interior observer to temporarily experience an "interior" of some kind? | |
| Jan 28 at 22:50 | history | edited | Rexcirus | CC BY-SA 4.0 |
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| Jan 28 at 22:43 | comment | added | Rexcirus | I replied to your comments in the answer. | |
| Jan 28 at 22:43 | history | edited | Rexcirus | CC BY-SA 4.0 |
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| Jan 28 at 20:41 | comment | added | Michael C. | Using the concept from Hartle and Hertog's article, just as the WdW wave function of the metric + the in-falling shell spreads out from the classical trajectory, in my gas cloud scenario the WdW wave function of the entire condensing cloud would have to do the same before the edge of the cloud reaches the Schwarzschild radius. At what radius would this wave function spread become significant? Near the would-be horizon or far out? | |
| Jan 28 at 18:41 | comment | added | Michael C. | I appreciate this answer and the references, but they ignore/evade the crux of my question by focusing on the collapse from the outside. I deliberately framed my question from the POV of a very low energy interior. In my scenario, at the moment a horizon would form according to GR, is 3.9x10^9 solar masses of low-density, low-energy gas across 6x10^30 km^3 supposed to instantly and simultaneously tunnel into a fuzzball microstate geometry on the boundary of the 76 AU sphere? | |
| Jan 28 at 15:30 | history | answered | Rexcirus | CC BY-SA 4.0 |