It's bigger on the inside: Tardis regions in spacetime and the expanding universeProfessors Rasanen, and Szybkab, of the University of Helsinki and the Jagellonian University at Krakow, together with Rasanen's graduate student Mikko Lavinto, decided to investigate another possibility.
The "standard cosmological model," which is the framework within which accelerated expansion requires dark energy, was developed in the 1920s and 1930s. The FLRW metric (named for Friedmann, Lemaître, Robertson and Walker, the major contributors) is an exact solution to Einstein's equations. It describes a strictly homogeneous, isotropic universe that can be expanding or contracting.
Strict homogeneity and strict isotropy means that the universe described by an FLRW metric looks the same at a given time from every point in space, at whatever distance or orientation you look. This is a universe in which galaxies, clusters of galaxies, sheets, walls, filaments, and voids do not exist. Not, then, very much like our own Universe, which appears to be rather homogeneous and isotropic when you look at distances greater than about a gigaparsec, but closer in it is nothing of the sort.
Physicists know a sequence of things happened in a particular order. They do not know, yet, what the clock rate for those events were, and for that they need to know how the vacuum quantizes events, how does the vacuum count. The vacuum would count differently if the environment at any one place were a bit different. So until we known the complete sequence, we do not know what the units of maximum entropy were along the path.
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