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File:Friedmann universes.svg




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This is a file from the Wikimedia Commons

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File:Friedmann universes.svg
Size of this PNG preview of this SVG file: 620 × 500 pixels. Other resolutions: 298 × 240 pixels | 595 × 480 pixels | 952 × 768 pixels | 1,270 × 1,024 pixels | 2,540 × 2,048 pixels.

Original file(SVG file, nominally 620 × 500 pixels, file size: 3 KB)





  • 2 Formulas
  • 3 See also
  • 4 Licensing
  • Summary

    Description
    English: Intended as a replacement for File:Universe.svg and File:Universos.gif.


    English: The age and ultimate fate of the universe can be determined by measuring the Hubble constant today and extrapolating with the observed value of the deceleration parameter, uniquely characterized by values of density parameters (ΩM for matter and ΩΛ for dark energy). A "closed universe" with ΩM > 1 and ΩΛ = 0 comes to an end in a Big Crunch and is considerably younger than its Hubble age. An "open universe" with ΩM ≤ 1 and ΩΛ = 0 expands forever and has an age that is closer to its Hubble age. For the accelerating universe with nonzero ΩΛ that we inhabit, the age of the universe is coincidentally very close to the Hubble age.
    Date
    Source Own work
    Author BenRG
    Permission
    (Reusing this file)
    Public domain

    This file supersedes the file Universe.svg. It is recommended to use this file rather than the other one.


    Reason why to use this file over the other file: "Improvements: better dash patterns, more accurate curves (actual solutions of the Friedmann equations, not hand-drawn)."

    Bahasa Indonesia  davvisámegiella  Deutsch  English  español  français  italiano  magyar  Nederlands  polski  svenska  македонски  മലയാളം  português do Brasil  русский  slovenščina  日本語  中文(简体)  中文(繁體)  farsi  +/−

    minor quality

    Formulas

    This diagram uses the following exact solutions to the Friedmann equations:

    )=\left({\tfrac {\Omega _{M}}{\Omega _{\Lambda }}}\sinh ^{2}\left({\tfrac {3}{2}}{\sqrt {\Omega _{\Lambda }}}H_{0}t\right)\right)^{1/3}&0<\Omega _{M}<1,\ \Omega _{\Lambda }=1-\Omega _{M}\end{cases}}}"> { a ( t ) = H 0 t Ω M = Ω Λ = 0 { a ( q ) = Ω M 2 ( 1 Ω M ) ( cosh q 1 ) t ( q ) = Ω M 2 H 0 ( 1 Ω M ) 3 / 2 ( sinh q q ) 0 < Ω M < 1 ,   Ω Λ = 0 a ( t ) = ( 3 2 H 0 t ) 2 / 3 Ω M = 1 ,   Ω Λ = 0 { a ( q ) = Ω M 2 ( Ω M 1 ) ( 1 cos q ) t ( q ) = Ω M 2 H 0 ( Ω M 1 ) 3 / 2 ( q sin q ) Ω M > 1 ,   Ω Λ = 0 a ( t ) = ( Ω M Ω Λ sinh 2 ( 3 2 Ω Λ H 0 t ) ) 1 / 3 0 < Ω M < 1 ,   Ω Λ = 1 Ω M {\displaystyle {\begin{cases}a(t)=H_{0}t&\Omega _{M}=\Omega _{\Lambda }=0\\{\begin{cases}a(q)={\tfrac {\Omega _{M}}{2(1-\Omega _{M})}}(\cosh q-1)\\t(q)={\tfrac {\Omega _{M}}{2H_{0}(1-\Omega _{M})^{3/2}}}(\sinh q-q)\end{cases}}&0<\Omega _{M}<1,\ \Omega _{\Lambda }=0\\a(t)=\left({\tfrac {3}{2}}H_{0}t\right)^{2/3}&\Omega _{M}=1,\ \Omega _{\Lambda }=0\\{\begin{cases}a(q)={\tfrac {\Omega _{M}}{2(\Omega _{M}-1)}}(1-\cos q)\\t(q)={\tfrac {\Omega _{M}}{2H_{0}(\Omega _{M}-1)^{3/2}}}(q-\sin q)\end{cases}}&\Omega _{M}>1,\ \Omega _{\Lambda }=0\\a(t)=\left({\tfrac {\Omega _{M}}{\Omega _{\Lambda }}}\sinh ^{2}\left({\tfrac {3}{2}}{\sqrt {\Omega _{\Lambda }}}H_{0}t\right)\right)^{1/3}&0<\Omega _{M}<1,\ \Omega _{\Lambda }=1-\Omega _{M}\end{cases}}} t)=\left({\tfrac {\Omega _{M}}{\Omega _{\Lambda }}}\sinh ^{2}\left({\tfrac {3}{2}}{\sqrt {\Omega _{\Lambda }}}H_{0}t\right)\right)^{1/3}&0<\Omega _{M}<1,\ \Omega _{\Lambda }=1-\Omega _{M}\end{cases}}}">

    See also

    Some of the shown models are implemented as an animation at Cosmos-animation.

    Licensing

    Public domain I, the copyright holder of this work, release this work into the public domain. This applies worldwide.
    In some countries this may not be legally possible; if so:
    I grant anyone the right to use this work for any purpose, without any conditions, unless such conditions are required by law.

    Captions

    Solutions of the Friedmann Equations (not hand drawn)

    Items portrayed in this file

    depicts

    some value

    23 September 2009

    image/svg+xml

    File history



    Click on a date/time to view the file as it appeared at that time.
    Date/TimeThumbnailDimensionsUserComment
    current22:09, 23 September 2009Thumbnail for version as of 22:09, 23 September 2009620 × 500 (3 KB)BenRGNimbus Roman doesn't have Greek letters; switch to DejaVu Serif
    22:02, 23 September 2009Thumbnail for version as of 22:02, 23 September 2009620 × 500 (3 KB)BenRG{{Information |Description=Intended as a replacement for File:Universe.svg and File:Universos.gif. Improvements: better dash patterns, more accurate curves (actual solutions of the Friedmann equations, not hand-drawn). |Source=Own work by upload



    The following pages on the English Wikipedia use this file (pages on other projects are not listed):

    Hubble's law

    Ultimate fate of the universe

    Talk:Ultimate fate of the universe/Archive 2

    Wikipedia:Reference desk/Archives/Science/2014 January 19


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    The following other wikis use this file:

    Usage on bg.wikipedia.org

    Потребител:NoelTomov/Съдбата на Вселената

    Съдбата на Вселената


    Usage on es.wikipedia.org

    Usuario:Karshan/Trabajando en


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    Universum


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    Soarta finală a universului


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    Konečný osud vesmíru


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    Evrenin nihai kaderi

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