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  2. Flatness problem - Wikipedia

    en.wikipedia.org/wiki/Flatness_problem

    The local geometry of the universe is determined by whether the relative density Ω is less than, equal to or greater than 1. From top to bottom: a spherical universe with greater than critical density (Ω>1, k>0); a hyperbolic, underdense universe (Ω<1, k<0); and a flat universe with exactly the critical density (Ω=1, k=0). The spacetime of ...

  3. Olbers's paradox - Wikipedia

    en.wikipedia.org/wiki/Olbers's_Paradox

    The redshift hypothesised in the Big Bang model would by itself explain the darkness of the night sky even if the universe were infinitely old. In the Steady state theory the universe is infinitely old and uniform in time as well as space. There is no Big Bang in this model, but there are stars and quasars at arbitrarily great distances.

  4. Flatness (cosmology) - Wikipedia

    en.wikipedia.org/wiki/Flatness_(cosmology)

    In cosmology, flatness is a property of a space without curvature. Such a space is called a "flat space" or Euclidean space [ citation needed ] . Whether the universe is “flat″ could determine its ultimate fate; whether it will expand forever, or ultimately collapse back into itself.

  5. Shape of the universe - Wikipedia

    en.wikipedia.org/wiki/Shape_of_the_universe

    The density parameter is the average density of the universe divided by the critical energy density, that is, the mass energy needed for a universe to be flat. Put another way, If Ω = 1, the universe is flat. If Ω > 1, there is positive curvature. If Ω < 1, there is negative curvature.

  6. Void (astronomy) - Wikipedia

    en.wikipedia.org/wiki/Void_(astronomy)

    There exist a number of ways for finding voids with the results of large-scale surveys of the universe. Of the many different algorithms, virtually all fall into one of three general categories. [27] The first class consists of void finders that try to find empty regions of space based on local galaxy density. [28]

  7. Cosmological principle - Wikipedia

    en.wikipedia.org/wiki/Cosmological_principle

    The perfect cosmological principle is an extension of the cosmological principle, and states that the universe is homogeneous and isotropic in space and time. In this view the universe looks the same everywhere (on the large scale), the same as it always has and always will. The perfect cosmological principle underpins steady state theory and ...

  8. Inhomogeneous cosmology - Wikipedia

    en.wikipedia.org/wiki/Inhomogeneous_cosmology

    An inhomogeneous cosmology is a physical cosmological theory (an astronomical model of the physical universe's origin and evolution) which, unlike the dominant cosmological concordance model, assumes that inhomogeneities in the distribution of matter across the universe affect local gravitational forces (i.e., at the galactic level) enough to skew our view of the Universe. [3]

  9. Taub–NUT space - Wikipedia

    en.wikipedia.org/wiki/Taub–NUT_space

    The underlying Taub space was found by Abraham Haskel Taub , and extended to a larger manifold by Ezra T. Newman, Louis A. Tamburino, and Theodore W. J. Unti , whose initials form the "NUT" of "Taub–NUT". Taub's solution is an empty space solution of Einstein's equations with topology R×S 3 and metric (or equivalently line element)