Speaker
Description
A homogeneous spherical cloud of pressureless matter ( M ) at rest will eventually collapse into a black hole characterized by its gravitational radius ( R_s = 2GM ). This forms what we term a Black Hole Universe (BHU). The BHU necessitates a boundary term to ensure that nothing can escape ( R_s ). This boundary term modifies Einstein’s field equations by adding a component that behaves identically to the observed cosmological constant (\Lambda = 3/R_s^2 ). Furthermore, we explore the quantum aspects of this boundary, offering a novel perspective on the Einstein-Rosen bridge. Our findings are supported by measurements of parity asymmetry in the Cosmic Microwave Background temperature perturbations, providing empirical evidence for this new theoretical framework.
