In SdS black hole holography, CV and CV2.0 complexities grow linearly while CA growth vanishes due to finite action, with matching rates between static patch and dS/CFT schemes.
The Holographic Principle for General Backgrounds
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abstract
We aim to establish the holographic principle as a universal law, rather than a property only of static systems and special space-times. Our covariant formalism yields an upper bound on entropy which applies to both open and closed surfaces, independently of shape or location. It reduces to the Bekenstein bound whenever the latter is expected to hold, but complements it with novel bounds when gravity dominates. In particular, it remains valid in closed FRW cosmologies and in the interior of black holes. We give an explicit construction for obtaining holographic screens in arbitrary space-times (which need not have a boundary). This may aid the search for non-perturbative definitions of quantum gravity in space-times other than AdS.
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In CEB-obeying models, postulated distributions of primordial black holes decaying to radiation can fit CMB data, account for all dark matter, and seed the early galaxies detected by JWST, with some Planck-scale remnants also contributing to DM.
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Holographic complexity of de-Sitter black holes
In SdS black hole holography, CV and CV2.0 complexities grow linearly while CA growth vanishes due to finite action, with matching rates between static patch and dS/CFT schemes.
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Can Primordial Black Holes Be Seeds for Early Galaxies in Models Satisfying the Covariant Entropy Bound?
In CEB-obeying models, postulated distributions of primordial black holes decaying to radiation can fit CMB data, account for all dark matter, and seed the early galaxies detected by JWST, with some Planck-scale remnants also contributing to DM.