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  2. Friedmann equations - Wikipedia

    en.wikipedia.org/wiki/Friedmann_equations

    The Friedmann equations, also known as the Friedmann–Lemaître ( FL) equations, are a set of equations in physical cosmology that govern the expansion of space in homogeneous and isotropic models of the universe within the context of general relativity. They were first derived by Alexander Friedmann in 1922 from Einstein's field equations of ...

  3. Equation of state (cosmology) - Wikipedia

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

    In an expanding universe, fluids with larger equations of state disappear more quickly than those with smaller equations of state. This is the origin of the flatness and monopole problems of the Big Bang : curvature has w = − 1 / 3 {\displaystyle w=-1/3} and monopoles have w = 0 {\displaystyle w=0} , so if they were around at the time of the ...

  4. Fermi paradox - Wikipedia

    en.wikipedia.org/wiki/Fermi_paradox

    The first aspect of the Fermi paradox is a function of the scale or the large numbers involved: there are an estimated 200–400 billion stars in the Milky Way (2–4 × 10 11) and 70 sextillion (7×10 22) in the observable universe.

  5. Lambda-CDM model - Wikipedia

    en.wikipedia.org/wiki/Lambda-CDM_model

    Astronomy portal. v. t. e. The Lambda-CDM, Lambda cold dark matter, or ΛCDM model is a mathematical model of the Big Bang theory with three major components: a cosmological constant, denoted by lambda (Λ), associated with dark energy. the postulated cold dark matter, denoted by CDM. ordinary matter. It is referred to as the standard model of ...

  6. Chronology of the universe - Wikipedia

    en.wikipedia.org/wiki/Chronology_of_the_universe

    From about 9.8 billion years of cosmic time, the universe's large-scale behavior is believed to have gradually changed for the third time in its history. Its behavior had originally been dominated by radiation (relativistic constituents such as photons and neutrinos) for the first 47,000 years, and since about 370,000 years of cosmic time, its ...

  7. Cosmological constant - Wikipedia

    en.wikipedia.org/wiki/Cosmological_constant

    v. t. e. In cosmology, the cosmological constant (usually denoted by the Greek capital letter lambda: Λ ), alternatively called Einstein's cosmological constant, is the constant coefficient of a term that Albert Einstein temporarily added to his field equations of general relativity. He later removed it; however, much later it was revived and ...

  8. Cosmic age problem - Wikipedia

    en.wikipedia.org/wiki/Cosmic_age_problem

    Cosmic age problem. The cosmic age problem was a historical problem in astronomy concerning the age of the universe. The problem was that at various times in the 20th century, the universe was estimated to be younger than the oldest observed stars. Estimates of the universe's age came from measurements of the current expansion rate of the ...

  9. The Scale of the Universe - Wikipedia

    en.wikipedia.org/wiki/The_Scale_of_the_Universe

    The Scale of the Universe is an interactive online visualization tool first created in 2010 by Cary and Michael Huang, two brothers from Moraga, California. Released on both Newgrounds and the Huang brothers' personal web page, it features a scrollbar that players can use to navigate through orders of magnitude and view various objects within such size ranges.

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