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  2. Scale factor (cosmology) - Wikipedia

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

    The scale factor is dimensionless, with counted from the birth of the universe and set to the present age of the universe: 13.799 ± 0.021 Gyr [4] giving the current value of as () or . The evolution of the scale factor is a dynamical question, determined by the equations of general relativity , which are presented in the case of a locally ...

  3. Lambda-CDM model - Wikipedia

    en.wikipedia.org/wiki/Lambda-CDM_model

    The fraction of the total energy density of our (flat or almost flat) universe that is dark energy, , is estimated to be 0.669 ± 0.038 based on the 2018 Dark Energy Survey results using Type Ia supernovae [7] or 0.6847 ± 0.0073 based on the 2018 release of Planck satellite data, or more than 68.3% (2018 estimate) of the mass–energy density ...

  4. The universe could undergo a 'catastrophic change' that could ...

    www.aol.com/universe-could-undergo-catastrophic...

    The groundbreaking simulation allowed scientists to better understand a phenomenon that could entirely change the structure of the universe – and about which little is still known

  5. Ultimate fate of the universe - Wikipedia

    en.wikipedia.org/wiki/Ultimate_fate_of_the_universe

    This suggests that the universe began very dense about 13.787 billion years ago, and it has expanded and (on average) become less dense ever since. [1] Confirmation of the Big Bang mostly depends on knowing the rate of expansion, average density of matter, and the physical properties of the mass–energy in the universe.

  6. Steady-state model - Wikipedia

    en.wikipedia.org/wiki/Steady-state_model

    On the other hand, the steady-state model says while the universe is expanding, it nevertheless does not change its appearance over time (the perfect cosmological principle). E.g., the universe has no beginning and no end. This required that matter be continually created in order to keep the universe's density from decreasing.

  7. Cosmic inflation - Wikipedia

    en.wikipedia.org/wiki/Cosmic_inflation

    [34] [35] It became known in the 1960s that the density of matter in the Universe was comparable to the critical density necessary for a flat universe (that is, a universe whose large-scale geometry is the usual Euclidean geometry, rather than a non-Euclidean hyperbolic or spherical geometry).

  8. Big Rip - Wikipedia

    en.wikipedia.org/wiki/Big_Rip

    In physical cosmology, the Big Rip is a hypothetical cosmological model concerning the ultimate fate of the universe, in which the matter of the universe, from stars and galaxies to atoms and subatomic particles, and even spacetime itself, is progressively torn apart by the expansion of the universe at a certain time in the future, until distances between particles will infinitely increase.

  9. Anthropic principle - Wikipedia

    en.wikipedia.org/wiki/Anthropic_principle

    The absurd universe: Our universe just happens to be the way it is. The unique universe: There is a deep underlying unity in physics that necessitates the Universe being the way it is. A Theory of Everything will explain why the various features of the Universe must have exactly the values that have been recorded.