Black-bounce to traversable wormhole

By Alex Simpson, Matt Visser. Journal of Cosmology and Astroparticle Physics, 2018

388 citations recorded by the source corpus.

So-called “regular black holes” are a topic currently of considerable interest in the general relativity and astrophysics communities. Herein we investigate a particularly interesting regular black hole spacetime described by the line element This spacetime neatly interpolates between the standard Schwarzschild black hole and the Morris-Thorne traversable wormhole; at intermediate stages passing through a black-bounce (into a future incarnation of the universe), an extremal null-bounce (into a future incarnation of the universe), and a traversable wormhole. As long as the parameter a is non-zero the geometry is everywhere regular, so one has a somewhat unusual form of “regular black hole”, where the “origin” r=0 can be either spacelike, null, or timelike. Thus this spacetime generalizes and broadens the class of “regular black holes” beyond those usually considered.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/88bc3401a614a0f7c2f3c319ac960c2b4f26edd9

How researchers see this paper

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In Astronomy and Astrophysics

1. J. Mazza
2. Edgardo Franzin
3. Hao Yang
4. Yang Guo
5. Stefano Liberati
6. Chen Lan
7. Y. Miao
8. D. Mattingly

In Nuclear and High Energy Physics

1. J. Mazza
2. Edgardo Franzin
3. Hao Yang
4. Yang Guo
5. Stefano Liberati
6. Chen Lan
7. Y. Miao
8. Giovanni Amelino-Camelia

In Statistical and Nonlinear Physics

1. Hao Yang
2. Yang Guo
3. Stefano Liberati
4. Chen Lan
5. Y. Miao
6. D. Mattingly
7. Giovanni Amelino-Camelia

Citations in the corpus

• A novel family of rotating black hole mimickers (2021, background): “Simpson and Visser [6–8] recently proposed a static and spherically symmetric metric that smoothly interpolates between these possibilities.”
• Regular Black Holes: A Short Topic Review (2023, methodology): “For the RBHs with two shape functions [7, 27, 98, 99], we apply a similar procedure to the above, that is, we expand both of shape functions (see Eq.”