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 electronuclear 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

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References

  1. ↑ D'Onofrio, Michela; 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.
  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. 1 2 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. 1 2 Ghiglieri, J.; Jackson, G.; Laine, M.; 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.
  8. ↑ L. D. McLerran; M. E. Shaposhnikov; N. Turok; 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.
  9. ↑ Morrissey, David E.; 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.
  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. Archived from the original on 2019-05-16. Retrieved 2020-07-14. 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. Archived from the original on 2019-06-06. Retrieved 2020-07-14. 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. S2CID   119416033.


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