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/

Zendy Plus

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

Zendy Tools

Zendy Open

Recently, various examples of asymptotically flat, rotating black holes (BHs)with synchronized hair have been explicitly constructed, including Kerr BHswith scalar or Proca hair, and Myers-Perry BHs with scalar hair and a mass gap,showing there is a general mechanism at work. All these solutions have beenfound numerically, integrating the fully non-linear field equations of motionfrom the event horizon outwards. Here, we address the spacetime geometry ofthese solutions inside the event horizon. Firstly, we provide arguments, withinlinear theory, that there is no regular inner horizon for these solutions.Then, we address this question fully non-linearly, using as a tractable modelfive dimensional, equal spinning, Myers-Perry hairy BHs. We find that, fornon-extremal solutions: $(1)$ the inside spacetime geometry in the vicinity ofthe event horizon is smooth and the equations of motion can be integratedinwards; $(2)$ before an inner horizon is reached, the spacetime curvaturegrows (apparently) without bound. In all cases, our results suggest the absenceof a smooth Cauchy horizon, beyond which the metric can be extended, for hairyBHs with synchronized hair.

Inside black holes with synchronized hair