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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We analyze in detail the geometry and dynamics of the cosmological regionarising in spherically symmetric black hole solutions of theEinstein-Maxwell-scalar field system with a positive cosmological constant.More precisely, we solve, for such a system, a characteristic initial valueproblem with data emulating a dynamic cosmological horizon. Our assumptions arefairly weak, in that we only assume that the data approaches that of asubextremal Reissner-Nordstr\"om-de Sitter black hole, without imposing anyrate of decay. We then show that the radius (of symmetry) blows up along anynull ray parallel to the cosmological horizon ("near" $i^+$), in such a waythat $r=+\infty$ is, in an appropriate sense, a spacelike hypersurface. We alsoprove a version of the Cosmic No-Hair Conjecture by showing that in the past ofany causal curve reaching infinity both the metric and the Riemann curvaturetensor asymptote those of a de Sitter spacetime. Finally, we discuss conditionsunder which all the previous results can be globalized.

Cosmic no-hair in spherically symmetric black hole spacetimes