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{{cosmology}}
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The '''accelerating universe''' is the observation that the universe appears to be [[Metric expansion of space|expanding]] at an increasing rate. In formal terms, this means that the [[Scale factor (cosmology)|cosmic scale factor]] <math>a(t)</math> has a positive [[second derivative]],<ref>{{cite book | last = Jones | first = Mark H. | coauthors = Robert J. Lambourne | title = An Introduction to Galaxies and Cosmology | publisher =Cambridge University Press | year=  2004 | page = [http://books.google.com/books?id=36K1PfetZegC&lpg=PP1&pg=PA244#v=onepage&q&f=false 244] | isbn = 978-0-521-83738-5 }}</ref> so that the velocity at which a distant galaxy is receding from us should be continuously increasing with time.<ref>[http://curious.astro.cornell.edu/question.php?number=575 Is the universe expanding faster than the speed of light?] (see final paragraph)</ref>
In 1998, observations of [[type Ia supernovae]] also suggested that the expansion of the [[universe]] has been accelerating<ref name="Riess 1998">{{cite journal|author=[[Adam Riess|Adam G. Riess]] ''et al.'' ([[Supernova Search Team]])|year=1998|title=Observational evidence from supernovae for an accelerating universe and a cosmological constant|journal=Astronomical J.|volume=116|issue=3|pages=1009–38|arxiv=astro-ph/9805201 |doi=10.1086/300499|bibcode=1998AJ....116.1009R}}</ref><ref name="Perlmutter 1999">{{cite journal|author=[[Saul Perlmutter|S. Perlmutter]] ''et al.'' (The [[Supernova Cosmology Project]])|journal=Astrophysical Journal|volume=517|issue=2|pages=565–86|year=1999|title=Measurements of Omega and Lambda from 42 high redshift supernovae|arxiv=astro-ph/9812133 |doi=10.1086/307221|bibcode=1999ApJ...517..565P}}</ref> since around [[redshift]] of z~0.5.<ref>Riess, A. G., et al. 2004, ''Astrophysical Journal'', 607, 665</ref> The 2006 [[Shaw Prize|Shaw Prize in Astronomy]] and the 2011 [[Nobel Prize in Physics]] were both awarded to [[Saul Perlmutter]], [[Brian P. Schmidt]], and [[Adam G. Riess]], who in 1998 as leaders of the [[Supernova Cosmology Project]] (Perlmutter) and the [[High-Z Supernova Search Team]] (Schmidt and Riess) discovered the accelerating expansion of the Universe through observations of distant ("High-Z") supernovae.<ref name="BBC">{{cite news|url=http://www.bbc.co.uk/news/science-environment-15165371|title=Nobel physics prize honours accelerating Universe find|publisher=BBC News|date=October 4, 2011}}</ref><ref>{{cite web|url=http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/# |title=The Nobel Prize in Physics 2011 |publisher=Nobelprize.org |date= |accessdate=2011-10-06}}</ref>


==Corroboration==
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After the initial discovery in 1998, these observations were corroborated by several independent sources: the [[cosmic microwave background radiation]] and [[Large-scale structure of the cosmos|large scale structure]],<ref>Spergel, D. N., et al. 2003, ''Astrophysical Journal Supplement'', 148, 175</ref> apparent size of [[baryon acoustic oscillation]]s,<ref name=real>[http://wigglez.swin.edu.au/site/prmay2011a.html Dark energy is real], Swinburne University of Technology, 19 May 2011</ref>  [[age of the universe]],<ref>Chaboyer, B., & Krauss, L. M. 2002, ''Astrophysical Journal Letters'', 567, L4</ref> as well as improved measurements of [[supernova]]e<ref>Wood-Vasey, W. M., et al.  2007, ''Astrophysical Journal'', 666, 694</ref><ref>Astier, P., et al. 2006, ''Astronomy and Astrophysics'', 447, 31
</ref> and X-ray properties of galaxy clusters.


==Explanatory models==
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Models attempting to explain accelerating expansion include some form of [[dark energy]], [[dark fluid]] or [[phantom energy]]. The most important property of dark energy is that it has negative [[pressure]] which is distributed relatively [[Homogeneity (physics)|homogeneously]] in space.  The simplest explanation for dark energy is that it is a [[cosmological constant]] or [[vacuum energy]]; this leads to the [[Lambda-CDM model]], which has generally been known as the Standard Model of Cosmology from 2003 through the present, since it is the simplest model in good agreement with a variety of recent observations.
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==Theories for the consequences to the universe==
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As the Universe expands, the density of radiation and ordinary and [[dark matter]] declines more quickly than the density of [[dark energy]] (see [[Equation of State (Cosmology)|equation of state]]) and, eventually, dark energy dominates. Specifically, when the scale of the universe doubles, the density of matter is reduced by a factor of 8, but the density of dark energy is nearly unchanged (it is exactly constant if the dark energy is a [[cosmological constant]]). 
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Current observations indicate that the dark energy density is already greater than the mass-energy density of radiation and matter (including [[dark matter]]). In models where dark energy is a [[cosmological constant]], the universe will expand exponentially with time from now on, coming closer and closer to a [[de Sitter space|de Sitter spacetime]]. In this scenario the time it takes for the linear size scale of the universe to expand to double its size is approximately 11.4 billion years.  Eventually all galaxies beyond our own [[local supercluster]] will [[redshift]] so far that it will become hard to detect them, and the distant universe will turn dark.
 
In other models, the density of dark energy changes with time.  In [[Quintessence (physics)|quintessence]] models it decreases, but more slowly than the energy density in ordinary matter and radiation. In [[phantom energy]] models it increases with time, leading to a [[Big Rip|big rip]].
 
==See also==
 
*[[High-z Supernova Search Team]]
*[[Supernova Cosmology Project]]
*[[Metric expansion of space]]
*[[List of multiple discoveries#21st century|List of multiple discoveries]]
*[[Cosmological constant]]
*[[Scale factor (cosmology)]]
*[[Friedmann–Lemaître–Robertson–Walker metric]]
 
==References==
{{Reflist}}
 
{{Breakthrough of the Year}}
 
[[Category:Physical cosmology]]
[[Category:Acceleration]]
[[Category:Universe]]
[[Category:Big Bang]]

Revision as of 21:14, 13 February 2014

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