English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Recent numerical relativity simulations within theEinstein--Maxwell--(charged-)Klein-Gordon (EMcKG) system have shown that thenon-linear evolution of a superradiantly unstable Reissner-Nordstr\"om blackhole (BH) enclosed in a cavity, leads to the formation of a BH with scalarhair. Perturbative evidence for the stability of such hairy BHs has beenindependently established, confirming they are the true endpoints of thesuperradiant instability. The same EMcKG system admits also charged scalarsoliton-type solutions, which can be either stable or unstable. Using numericalrelativity techniques, we provide evidence that the time evolution of some ofthese $\textit{unstable}$ solitons leads, again, to the formation of a hairyBH. In some other cases, unstable solitons evolve into a (bald)Reissner-Nordstr\"om BH. These results establish that the system admits twodistinct channels to form hairy BHs at the threshold of superradiance: growinghair from an unstable (bald) BH, or growing a horizon from an unstable(horizonless) soliton. Some parallelism with the case of asymptotically flatboson stars and Kerr BHs with scalar hair is drawn.

Dynamical formation of a hairy black hole in a cavity from the decay of unstable solitons