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Vaidya spacetimes, black-bounces, and traversable wormholes

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arxiv 1902.04232 v3 pith:UHMNHD34 submitted 2019-02-12 gr-qc

Alex Simpson (Victoria University of Wellington) , Prado Martin-Moruno (Universidad Complutense de Madrid) , Matt Visser (Victoria University of Wellington) This is my paper · ORCID
classification gr-qc
keywords black-bouncewormholeleftmetricrightspacetimetimetraversable
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abstract

We consider a non-static evolving version of the regular "black-bounce"/traversable wormhole geometry recently introduced in JCAP02(2019)042 [arXiv:1812.07114 [gr-qc]]. We first re-write the static metric using Eddington-Finkelstein coordinates, and then allow the mass parameter $m$ to depend on the null time coordinate (a la Vaidya). The spacetime metric is \[ ds^{2}=-\left(1-\frac{2m(w)}{\sqrt{r^{2}+a^{2}}}\right)dw^{2}-(\pm 2 \,dw \,dr) +\left(r^{2}+a^{2}\right)\left(d\theta^{2}+\sin^{2}\theta \;d\phi^{2}\right). \] Here $w=\{u,v\}$ denotes the $\{outgoing,ingoing\}$ null time coordinate; representing $\{retarded,advanced\}$ time. This spacetime is still simple enough to be tractable, and neatly interpolates between Vaidya spacetime, a black-bounce, and a traversable wormhole. We show how this metric can be used to describe several physical situations of particular interest, including a growing black-bounce, a wormhole to black-bounce transition, and the opposite black-bounce to wormhole transition.

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Cited by 5 Pith papers

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