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In [[physical cosmology]], the '''electroweak epoch''' was the period in the evolution of the early universe when the temperature of the universe had fallen enough that the [[strong force]] separated from the [[electroweak]] interaction, but was high enough for [[electromagnetism]] and the [[weak interaction]] to remain merged into a single [[electroweak interaction]] (above energies of about 246 [[GeV]]<!-- IF THIS IS CHANGED, PLEASE ALSO UPDATE THE SAME INFO AT [[Chronology of the universe]], [[Electroweak scale]], [[Electroweak interaction]]. THANK YOU. -->,<ref>The particular number 246 GeV is taken to be the [[vacuum expectation value]] <math>v = (G_F \sqrt{2})^{-1/2}</math> of the [[Higgs field]] (where <math>G_F</math> is the [[Fermi coupling constant]]).</ref>{{verify source|date=March 2018}}). Some cosmologists place this event at the start of the [[inflationary epoch]], approximately 10<sup>−36</sup> seconds after the [[Big Bang]].<ref>Ryden B: "Introduction to Cosmology", pg. 196 Addison-Wesley 2003</ref><ref>{{cite book | last = Allday | first = Jonathan | title = Quarks, Leptons and the Big Bang | publisher = [[Taylor & Francis]] | year = 2002 | isbn = 978-0-7503-0806-9 |page = 334}}</ref><ref>[http://sciexplorer.blogspot.com/2011/01/our-universe-part-6-electroweak-epoch.html Our Universe Part 6: Electroweak Epoch], Scientific Explorer</ref> Others place it at approximately 10<sup>−32</sup> seconds after the Big Bang when the potential energy of the [[inflaton]] field that had driven the [[cosmic inflation|inflation]] of the universe during the inflationary epoch was released, filling the universe with a dense, hot [[quark–gluon plasma]].<ref>[http://nicadd.niu.edu/~bterzic/PHYS652/Lecture_13.pdf Lecture 13: History of the Very Early Universe], Dr. Balša Terzić, Northern Illinois Center for Accelerator and Detector Development</ref> Particle interactions in this phase were energetic enough to create large numbers of [[exotic particle]]s, including [[W and Z bosons]] and [[Higgs boson]]s. As the universe expanded and cooled, interactions became less energetic and when the universe was about 10<sup>−12</sup> seconds old, W and Z bosons ceased to be created. The remaining W and Z bosons decayed quickly, and the weak interaction became a short-range force in the following [[quark epoch]]. |
In [[physical cosmology]], the '''electroweak epoch''' was the period in the evolution of the early universe when the temperature of the universe had fallen enough that the [[strong force]] separated from the [[electroweak]] interaction, but was high enough for [[electromagnetism]] and the [[weak interaction]] to remain merged into a single [[electroweak interaction]] (above energies of about 246 [[GeV]]<!-- IF THIS IS CHANGED, PLEASE ALSO UPDATE THE SAME INFO AT [[Chronology of the universe]], [[Electroweak scale]], [[Electroweak interaction]]. THANK YOU. -->,<ref>The particular number 246 GeV is taken to be the [[vacuum expectation value]] <math>v = (G_F \sqrt{2})^{-1/2}</math> of the [[Higgs field]] (where <math>G_F</math> is the [[Fermi coupling constant]]).</ref>{{verify source|date=March 2018}}). Some cosmologists place this event at the start of the [[inflationary epoch]], approximately 10<sup>−36</sup> seconds after the [[Big Bang]].<ref>Ryden B: "Introduction to Cosmology", pg. 196 Addison-Wesley 2003</ref><ref>{{cite book | last = Allday | first = Jonathan | title = Quarks, Leptons and the Big Bang | publisher = [[Taylor & Francis]] | year = 2002 | isbn = 978-0-7503-0806-9 |page = 334}}</ref><ref>[http://sciexplorer.blogspot.com/2011/01/our-universe-part-6-electroweak-epoch.html Our Universe Part 6: Electroweak Epoch], Scientific Explorer</ref> Others place it at approximately 10<sup>−32</sup> seconds after the Big Bang when the potential energy of the [[inflaton]] field that had driven the [[cosmic inflation|inflation]] of the universe during the inflationary epoch was released, filling the universe with a dense, hot [[quark–gluon plasma]].<ref>[http://nicadd.niu.edu/~bterzic/PHYS652/Lecture_13.pdf Lecture 13: History of the Very Early Universe], Dr. Balša Terzić, Northern Illinois Center for Accelerator and Detector Development</ref> Particle interactions in this phase were energetic enough to create large numbers of [[exotic particle]]s, including [[W and Z bosons]] and [[Higgs boson]]s. As the universe expanded and cooled, interactions became less energetic and when the universe was about 10<sup>−12</sup> seconds old, W and Z bosons ceased to be created. The remaining W and Z bosons decayed quickly, and the weak interaction became a short-range force in the following [[quark epoch]]. |
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The physics of the electroweak epoch is less speculative and much better understood than the physics of previous periods of the early universe. The existence of W, Z, and Higgs bosons has been demonstrated, and other{{Which|date=April 2012}} predictions of electroweak theory have been experimentally verified. |
The physics of the electroweak epoch is less speculative and much better understood than the physics of previous periods of the early universe. The existence of W, Z, and Higgs bosons has been demonstrated, and other{{Which|date=April 2012}} predictions of electroweak theory have been experimentally verified. Whether the transition from this epoch was a continuous crossover or a first-order phase change is disputed, and this influences the possibility of [[Baryogenesis#Baryogenesis within the Standard Model (Electroweak Baryogenesis)|baryogenesis within the Standard Model]].<ref>{{cite journal |last1=Bergerhoff |first1=Bastian |last2=Wetterich |first2=Christof |title=Electroweak Phase Transition in the Early Universe? |date=1998 |pages=211–240 |doi=10.1007/978-94-011-5046-0_6 |url=https://link.springer.com/chapter/10.1007/978-94-011-5046-0_6 |accessdate=20 June 2019 |publisher=Springer Netherlands |language=en}}</ref> |
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==See also== |
==See also== |
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Revision as of 01:42, 23 June 2019
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In physical cosmology, the electroweak epoch was the period in the evolution of the early universe when the temperature of the universe had fallen enough that the strong force separated from the electroweak interaction, but was high enough for electromagnetism and the weak interaction to remain merged into a single electroweak interaction (above energies of about 246 GeV,[1][verification needed]). Some cosmologists place this event at the start of the inflationary epoch, approximately 10−36 seconds after the Big Bang.[2][3][4] Others place it at approximately 10−32 seconds after the Big Bang when the potential energy of the inflaton field that had driven the inflation of the universe during the inflationary epoch was released, filling the universe with a dense, hot quark–gluon plasma.[5] Particle interactions in this phase were energetic enough to create large numbers of exotic particles, including W and Z bosons and Higgs bosons. As the universe expanded and cooled, interactions became less energetic and when the universe was about 10−12 seconds old, W and Z bosons ceased to be created. The remaining W and Z bosons decayed quickly, and the weak interaction became a short-range force in the following quark epoch.
The physics of the electroweak epoch is less speculative and much better understood than the physics of previous periods of the early universe. The existence of W, Z, and Higgs bosons has been demonstrated, and other[which?] predictions of electroweak theory have been experimentally verified. Whether the transition from this epoch was a continuous crossover or a first-order phase change is disputed, and this influences the possibility of baryogenesis within the Standard Model.[6]
See also
References
- ^ The particular number 246 GeV is taken to be the vacuum expectation value of the Higgs field (where is the Fermi coupling constant).
- ^ Ryden B: "Introduction to Cosmology", pg. 196 Addison-Wesley 2003
- ^ Allday, Jonathan (2002). Quarks, Leptons and the Big Bang. Taylor & Francis. p. 334. ISBN 978-0-7503-0806-9.
- ^ Our Universe Part 6: Electroweak Epoch, Scientific Explorer
- ^ Lecture 13: History of the Very Early Universe, Dr. Balša Terzić, Northern Illinois Center for Accelerator and Detector Development
- ^ Bergerhoff, Bastian; Wetterich, Christof (1998). "Electroweak Phase Transition in the Early Universe?". Springer Netherlands: 211–240. doi:10.1007/978-94-011-5046-0_6. Retrieved 20 June 2019.
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- Greene, Brian (2005). The Fabric of the Cosmos: Space, Time, and the Texture of Reality. Penguin Books Ltd. Bibcode:2004fcst.book.....G. ISBN 978-0-14-101111-0.
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