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| <!-- Don't re-add [[File:Big rip.gif]] without saying why on the talk page. There are 4 people there saying it's better not to have the picture and no one has yet given a reason why it should be here. URL: https://secure.wikimedia.org/wikipedia/en/wiki/Talk:Big_Rip#Picture_is_Confusing -->
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| The '''Big Rip''' is a [[physical cosmology|cosmological]] [[hypothesis]] first published in 2003, about the [[ultimate fate of the universe]], in which the matter of the [[universe]], from stars and galaxies to atoms and subatomic particles, is progressively torn apart by the [[metric expansion of space|expansion of the universe]] at a certain time in the future. According to the hypothesis, the [[Scale factor (cosmology)|scale factor]] of the universe and with it all distances in the universe will become [[Infinity|infinite]] at a [[Wikt:finite|finite]] time in the future. It is important to note that the possibility of sudden singularities and crunch or rip singularities at late times occur only for hypothetical matter with implausible physical properties. <ref> Ellis, George F. R., R. Maartens, and M. A. H. MacCallum. Relativistic Cosmology. Cambridge: Cambridge UP, 2012. 146-47. Print. </ref>
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| ==Definition and overview==
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| The hypothesis relies crucially on the type of [[dark energy]] in the [[universe]]. The key value is the [[equation of state (cosmology)|equation of state]] parameter <math>w</math>, the [[ratio]] between the dark energy pressure and its [[energy density]]. At <math>w</math> < −1, the universe will eventually be pulled apart. Such energy is called [[phantom energy]], an extreme form of [[quintessence (physics)|quintessence]].
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| A universe dominated by phantom energy expands at an ever-increasing rate. However, this implies that the size of the [[observable universe]] is continually shrinking; the distance to the edge of the observable universe which is moving away at the speed of light from any point moves ever closer. When the size of the observable universe becomes smaller than any particular structure, no interaction by any of the fundamental forces ([[Gravity|gravitational]], [[Electromagnetism|electromagnetic]], [[Weak nuclear force|weak]], or [[Strong interaction|strong]]) can occur between the most remote parts of the structure. When these interactions become impossible, the structure is "ripped apart". The model implies that after a finite time there will be a final singularity, called the "Big Rip", in which all distances diverge to infinite values.
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| The authors of this hypothesis, led by Robert Caldwell of [[Dartmouth College]], calculate the time from the present to the end of the universe as we know it for this form of energy to be
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| <math>t_{rip} - t_{0} \approx \frac{2}{3|1+w|H_0\sqrt{1-\Omega_m}}</math>
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| where <math>w</math> is defined above, H<sub>0</sub> is [[Hubble's constant]] and Ω<sub>m</sub> is the present value of the density of all the matter in the universe.
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| In their paper, the authors consider an example with <math>w</math> = −1.5, H<sub>0</sub> = 70 km/s/Mpc and Ω<sub>m</sub> = 0.3, in which case the end of the universe is approximately 22 billion years from the present. This is not considered a prediction, but a hypothetical example. The authors note that evidence indicates <math>w</math> to be very close to −1 in our universe, which makes <math>w</math> the dominating term in the equation. The closer that the quantity (1 + <math>w</math>) is to zero, the closer the denominator is to zero and the further the Big Rip is in the future. If <math>w</math> were exactly equal to −1, the Big Rip could not happen, regardless of the values of H<sub>0</sub> or Ω<sub>m</sub>.
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| In their scenario for <math>w</math> = −1.5, the [[galaxies]] would first be separated from each other. About 60 million years before the end, gravity would be too weak to hold the [[Milky Way]] and other individual galaxies together. Approximately three months before the end, the [[solar system]] (or systems similar to our own at this time, as the fate of our own solar system 7.5 billion years in the future is questionable) would be gravitationally unbound. In the last minutes, stars and planets would be torn apart, and an instant before the end, [[atom]]s would be destroyed.<ref>{{cite journal
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| | doi = 10.1103/PhysRevLett.91.071301
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| | last = Caldwell | first = Robert R.
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| | coauthors = Kamionkowski, Marc and Weinberg, Nevin N.
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| | title = Phantom Energy and Cosmic Doomsday
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| | journal = Physical Review Letters
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| | volume = 91
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| | pages = 071301
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| | year = 2003
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| | id =
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| | pmid=12935004
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| | arxiv=astro-ph/0302506
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| | bibcode=2003PhRvL..91g1301C
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| | issue = 7
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| }}</ref>
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| ==Experimental data==
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| According to the latest cosmological data available, the uncertainties are still too large to discriminate among the three cases <math>w</math> < −1, <math>w</math> = −1, and <math>w</math> > −1.<ref>http://wmap.gsfc.nasa.gov/news/</ref><ref>{{Cite journal | bibcode = 2008MNRAS.383..879A | title = Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters | author1 = Allen | first1 = S. W. | last2 = Rapetti | first2 = D. A. | last3 = Schmidt | first3 = R. W. | last4 = Ebeling | first4 = H. | last5 = Morris | first5 = R. G. | last6 = Fabian | first6 = A. C. | volume = 383 | year = 2008 | pages = 879 | journal = Monthly Notices of the Royal Astronomical Society | doi = 10.1111/j.1365-2966.2007.12610.x | issue = 3|arxiv = 0706.0033 }}</ref>
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| == See also ==
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| {{Portal box|Astronomy|Space|Solar System}}
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| * [[List of astronomical topics]]
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| * [[Accelerating universe]]
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| * [[Heat-death of the Universe]]
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| * [[Big Crunch]]
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| * [[Big Bounce]]
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| * [[Big Freeze]]
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| * [[Entropy (arrow of time)]]
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| * [[Ultimate fate of the Universe]]
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| * [[Phantom energy]]
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| * [[Cyclic Model]]
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| * [[Dark energy]]
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| ==References==
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| {{Reflist}}
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| ==External links==
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| * [http://www.nytimes.com/2004/02/17/science/from-space-a-new-view-of-doomsday.html?pagewanted=all&src=pm]
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| {{Doomsday}}
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| [[Category:Physical cosmology]]
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| [[Category:Teleology]]
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| [[Category:Eschatology]]
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| [[Category:2003 introductions]]
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