Connecting horizon pixels and interior voxels of a black hole

TL;DR

This paper explores how the interior structure of a black hole can be inferred from its horizon by proposing a holographic relationship between horizon pixels and interior voxels, especially in models with a singularity-free interior.

Contribution

It introduces a novel holographic framework linking horizon and interior degrees of freedom in black holes with non-classical interiors, challenging traditional no-hair limitations.

Findings

Horizon pixels can be mapped to interior voxels via holography.

Black hole entropy can be derived from a statistical ensemble of interior voxels.

A de Sitter core model illustrates the interior-structure inference.

Abstract

In this paper we discuss to what extent one can infer details of the interior structure of a black hole based on its horizon. Recalling that black hole thermal properties are connected to the non-classical nature of gravity, we circumvent the restrictions of the no hair theorem by postulating that the black hole interior is singularity free due to violations of the usual energy conditions. Further these conditions allow one to establish a one-to-one, holographic projection between Planckian areal "bits" on the horizon and "voxels", representing the gravitational degrees of freedom in the black hole interior. We illustrate the repercussions of this idea by discussing an example of the black hole interior consisting of a de Sitter core postulated to arise from the local graviton quantum vacuum energy. It is shown that the black hole entropy can emerge as the statistical entropy of a gas of voxels.