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  2. Cosmological principle - Wikipedia

    en.wikipedia.org/wiki/Cosmological_principle

    In modern physical cosmology, the cosmological principle is the notion that the spatial distribution of matter in the universe is uniformly isotropic and homogeneous when viewed on a large enough scale, since the forces are expected to act equally throughout the universe on a large scale, and should, therefore, produce no observable inequalities in the large-scale structuring over the course ...

  3. Friedmann equations - Wikipedia

    en.wikipedia.org/wiki/Friedmann_equations

    The first Friedmann equation is often seen in terms of the present values of the density parameters, that is [6] =, +, +, +,. Here Ω 0,R is the radiation density today (when a = 1 ), Ω 0,M is the matter ( dark plus baryonic ) density today, Ω 0, k = 1 − Ω 0 is the "spatial curvature density" today, and Ω 0,Λ is the cosmological constant ...

  4. Equation of state (cosmology) - Wikipedia

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

    These problems are solved by cosmic inflation which has . Measuring the equation of state of dark energy is one of the largest efforts of observational cosmology . By accurately measuring w {\displaystyle w} , it is hoped that the cosmological constant could be distinguished from quintessence which has w ≠ − 1 {\displaystyle w\neq -1} .

  5. Lambda-CDM model - Wikipedia

    en.wikipedia.org/wiki/Lambda-CDM_model

    The values of these six parameters are mostly not predicted by theory (though, ideally, they may be related by a future "Theory of Everything"), except that most versions of cosmic inflation predict the scalar spectral index should be slightly smaller than 1, consistent with the estimated value 0.96. The parameter values, and uncertainties, are ...

  6. Hubble's law - Wikipedia

    en.wikipedia.org/wiki/Hubble's_law

    These values arise from fitting a combination of WMAP and other cosmological data to the simplest version of the ΛCDM model. If the data are fit with more general versions, H 0 tends to be smaller and more uncertain: typically around 67 ± 4 (km/s)/Mpc although some models allow values near 63 (km/s)/Mpc. [145] 2010 71.0 ± 2.5: WMAP only (7 ...

  7. Cosmological constant - Wikipedia

    en.wikipedia.org/wiki/Cosmological_constant

    Using the values known in 2018 and Planck units for Ω Λ = 0.6889 ± 0.0056 and the Hubble constant H 0 = 67.66 ± 0.42 (km/s)/Mpc = (2.192 7664 ± 0.0136) × 10 −18 s −1, Λ has the value of = = = where is the Planck length. A positive vacuum energy density resulting from a cosmological constant implies a negative pressure, and vice versa.

  8. 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).

  9. 99Vidas - Wikipedia

    en.wikipedia.org/wiki/99Vidas

    99Vidas (Portuguese for "99 Lives") is a retro-styled side-scrolling beat 'em up video game developed and published by Brazilian [2] studio QuByte Interactive. It was first released for Microsoft Windows, macOS, and Linux in late 2016, followed by PlayStation 3, PlayStation 4 and PlayStation Vita in 2017. [3]