 Others (e.g., Davies 1994) have thought inflation provides a kind of entropy-increasing behavior—again, given the sort of matter content we have in our universe. The inflationary model is an alternative of sorts to the standard big bang model, although by now it is so well entrenched in the cosmology community that it really deserves the tag “standard”. In this scenario, the universe is very early in a quantum state called a “false vacuum”, a state with a very high energy density and negative pressure. Gravity acts like Einstein’s cosmological constant, so that it is repulsive rather than attractive. Under this force the universe enters a period of exponential inflation, with geometry resembling de Sitter space. When this period ends any initial inhomogeneities will have been smoothed to insignificance. At this point ordinary stellar evolution begins. Loosely associating gravitational homogeneity with low-entropy and inhomogeneity with higher entropy, inflation is arguably a source of a low entropy “initial” condition.