标题： TO_BE_TRANSLATED: Geometric distances between closed universes 显示英文标题

标题： Geometric distances between closed universes

摘要： TO_BE_TRANSLATED: The large-scale structure of the universe is well-approximated by the Friedmann equations, parameterised by several energy densities which can be observationally inferred. A natural question to ask is: how different would the universe be if these densities took on other values? While there are many ways this can be approached depending on interpretation and mathematical rigour, we attempt an answer by building a "history space" of different cosmologies. A metric is introduced after overcoming technical hurdles related to Lorentzian signature and infinite volume, at least for topologically-closed cases. Geodesics connecting two points on the superspace are computed to express how distant -- in a purely geometric sense -- two universes are. Age can be treated as a free parameter in such an approach, leading to a more general mathematical construct relative to geometrodynamical configuration-space. Connections to bubble inflation and phase transitions are explored. 显示英文摘要

摘要： The large-scale structure of the universe is well-approximated by the Friedmann equations, parameterised by several energy densities which can be observationally inferred. A natural question to ask is: how different would the universe be if these densities took on other values? While there are many ways this can be approached depending on interpretation and mathematical rigour, we attempt an answer by building a "history space" of different cosmologies. A metric is introduced after overcoming technical hurdles related to Lorentzian signature and infinite volume, at least for topologically-closed cases. Geodesics connecting two points on the superspace are computed to express how distant -- in a purely geometric sense -- two universes are. Age can be treated as a free parameter in such an approach, leading to a more general mathematical construct relative to geometrodynamical configuration-space. Connections to bubble inflation and phase transitions are explored.