Not quite a black hole
By B. Holdom, Jing Ren. 2016
134 citations recorded by the source corpus.
Astrophysical black hole candidates, although long thought to have a horizon, could be horizonless ultracompact objects. This intriguing possibility is motivated by the black hole information paradox and a plausible fundamental connection with quantum gravity. Asymptotically free quadratic gravity is considered here as the UV completion of general relativity. A classical theory that captures its main features is used to search for solutions as sourced by matter. We find that sufficiently dense matter produces a novel horizonless configuration, the 2-2-hole, which closely matches the exterior Schwarzschild solution down to about a Planck proper length of the would-be horizon. The 2-2-hole is characterized by an interior with a shrinking volume and a seemingly innocuous timelike curvature singularity. The interior also has a novel scaling behavior with respect to the physical mass of the 2-2-hole. This leads to an extremely deep gravitational potential in which particles get efficiently trapped via collisions. As a generic static solution, the 2-2-hole may then be the nearly black end point of gravitational collapse. There is a considerable time delay for external probes of the 2-2-hole interior, and this determines the spacing of echoes in a postmerger gravitational wave signal.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/5f6fd592c345039a0cf2837bcd9a2578c45b11ef
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Citations in the corpus
- Phenomenological aspects of black holes beyond general relativity (2018, background): “[184] Bob Holdom and Jing Ren, “Not quite a black hole,” Phys.”
- Quadratic Gravity (2018, background): “Holdom and Ren [107] considered the creation of a static spherically symmetric solution generated by a thin spherically symmetric shell of matter; when the shell radius l .”
- Tests for the existence of black holes through gravitational wave echoes (2017, background): “In these models, the parameter is naturally of the order ∼ 10−39 − 10−46 for masses in the range 10−10(8)M , or even smaller in some models [27].”