Electroweak epoch

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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 the critical temperature for electroweak symmetry breaking (159.5±1.5 GeV [1] in the Standard Model of particle physics). Some cosmologists place the electroweak epoch 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 at observable rates.[citation needed] The remaining W and Z bosons decayed quickly, and the weak interaction became a short-range force in the following quark epoch.

The electroweak epoch ended with an electroweak phase transition, the nature of which is unknown. If first order, this could source a gravitational wave background.[6][7] The electroweak phase transition is also a potential source of baryogenesis,[8][9] provided the Sakharov conditions are satisfied.[10]

In the minimal Standard Model, the transition during the electroweak epoch was not a first- or a second-order phase transition but a continuous crossover, preventing any baryogenesis,[11][12] or the production of an observable gravitational wave background.[6] [7] However many extensions to the Standard Model including supersymmetry and the two-Higgs-doublet model have a first-order electroweak phase transition (but require additional CP violation).[citation needed]

See also[edit]

References[edit]

  1. ^ D'Onofrio, Michela and Rummukainen, Kari (2016). "Standard model cross-over on the lattice". Phys. Rev. D. 93 (2): 025003. arXiv:1508.07161. Bibcode:2016PhRvD..93b5003D. doi:10.1103/PhysRevD.93.025003. hdl:10138/159845. S2CID 119261776.CS1 maint: multiple names: authors list (link)
  2. ^ Ryden, B. (2003). Introduction to Cosmology. Addison-Wesley. p. 196. ISBN 0-8053-8912-1.
  3. ^ Allday, Jonathan (2002). Quarks, Leptons and the Big Bang. Taylor & Francis. p. 334. ISBN 978-0-7503-0806-9.
  4. ^ Our Universe Part 6: Electroweak Epoch, Scientific Explorer
  5. ^ Lecture 13: History of the Very Early Universe Archived 2012-03-27 at the Wayback Machine, Dr. Balša Terzić, Northern Illinois Center for Accelerator and Detector Development
  6. ^ a b Caprini, Chiara; et al. (2020). "Detecting gravitational waves from cosmological phase transitions with LISA: an update". Journal of Cosmology and Astroparticle Physics. 2020 (3): 024. arXiv:1910.13125. Bibcode:2020JCAP...03..024C. doi:10.1088/1475-7516/2020/03/024. S2CID 204950387.
  7. ^ a b Ghiglieri, J. and Jackson, G. and Laine, M. and Zhu, Y. (2020). "Gravitational wave background from Standard Model physics: Complete leading order". Journal of High Energy Physics. 2020 (7): 092. arXiv:2004.11392. Bibcode:2020JHEP...07..092G. doi:10.1007/JHEP07(2020)092. S2CID 216144470.CS1 maint: multiple names: authors list (link)
  8. ^ L. D. McLerran, M. E. Shaposhnikov, N. Turok and M. B. Voloshin (1991). "Why the baryon asymmetry of the universe is approximately 10**-10". Phys. Lett. B. 256: 451–456. doi:10.1016/0370-2693(91)91794-V.CS1 maint: multiple names: authors list (link)
  9. ^ Morrissey, David E. and Ramsey-Musolf, Michael J. (2012). "Electroweak baryogenesis". New J. Phys. 14 (12): 12500. arXiv:1206.2942. Bibcode:2012NJPh...14l5003M. doi:10.1088/1367-2630/14/12/125003. S2CID 119230032.CS1 maint: multiple names: authors list (link)
  10. ^ A. D. Sakharov (1967). "Violation of CP invariance, C asymmetry, and baryon asymmetry of the universe". Journal of Experimental and Theoretical Physics Letters. 5: 24–27. and in Russian, A. D. Sakharov (1967). "Violation of CP invariance, C asymmetry, and baryon asymmetry of the universe". ZhETF Pis'ma. 5: 32–35. republished as A. D. Sakharov (1991). "Violation of CP invariance, C asymmetry, and baryon asymmetry of the universe". Soviet Physics Uspekhi (in Russian and English). 34 (5): 392–393. Bibcode:1991SvPhU..34..392S. doi:10.1070/PU1991v034n05ABEH002497.
  11. ^ Bergerhoff, Bastian; Wetterich, Christof (1998). "Electroweak Phase Transition in the Early Universe?". Current Topics in Astrofundamental Physics: Primordial Cosmology. Springer Netherlands. pp. 211–240. arXiv:hep-ph/9611462. doi:10.1007/978-94-011-5046-0_6. ISBN 978-94-010-6119-3. S2CID 13949582.
  12. ^ Kajantie, Keijo; et al. (1996). "The Electroweak Phase Transition: A Non-Perturbative Analysis". Nucl. Phys. B. 466 (1–2): 189–258. arXiv:hep-lat/9510020. Bibcode:1996NuPhB.466..189K. doi:10.1016/0550-3213(96)00052-1.