Abstract
The evolution of the vacuum component of the Universe is studied in both the quantum and classical regimes. Our Universe has emerged as a result of a tunneling process, beginning with an oscillating mode and passing on to a Friedmann mode, and it very probably had a high symmetry for the Planck parameters. In the first fractions of a second (the quantum regime), as it cooled, the vacuum component of the Universe lost its high degree of symmetry due to phase transitions; i.e., its positive energy density was subject to negative contributions from quantum field condensates (by 78 orders of magnitude). After the last (quark-hadron) phase transition, the vacuum energy “froze.” At this time (10−6 s), the vacuum energy density can be calculated using the formula of Zel’dovich and substituting the mean values of the pseudo-Goldstone boson (π-mesons) masses characterizing the chromodynamic vacuum. Chiral symmetrywas lost at that time. The dynamics of the equilibrium vacuum after its “hardening” is considered using the holographic principle. During the next 4 × 1017 s (the classical regime), the vacuum component of the Universe was reduced by 45 orders of magnitude due to the creation of new quantum states during its expansion. It is possible to solve the cosmological-constant problem using the holographic principle, since the 123 problematic orders of magnitude disappear in usual physical processes. The vacuum energy density is also calculated in the classical regime to a redshift of 1011 using a “cosmological calculator.”
Similar content being viewed by others
References
A. Einstein, Sitzungsber. Preuss. Akad. Wiss., p. 142 (1917).
S. Weinberg, Rev.Mod. Phys. 61, 1 (1989).
S. Carroll, Living Rev. Relat. 4, 1 (2004); arXiv:astroph/0004075 (2000).
V. Sahni and A. Starobinsky, Int. J. Mod. Phys. D 9, 371 (2000).
P. Peebles and B. Ratra, Rev. Mod. Phys. 75, 559 (2003).
T. Padmanabhan, Phys. Rep. 380, 235 (2003).
R. Bousso, Gen. Relat. Gravit. 40, 607 (2008); arXiv:0708.4231 [astro-ph] (2007).
J. A. Frieman, M. S. Turner, and D. Huterer, Ann. Rev. Astron. Astrophys. 46, 385 (2008).
L. Marochnik, D. Usikov, and G. Vereshkov, arXiv:0811.4484 [gr-qc] (2008).
V. V. Burdyuzha, Astron. Rep. 53, 381 (2009).
V. V. Burdyuzha, Phys. Usp. 50, 819 (2010).
R. Peccei, J. Sola, and C. Wetterich, Phys. Lett. B 195, 183 (1987).
D. Arnaudon, C. Bachas, V. Rivasseau, and P. Vegreville, Phys. Lett. B 195, 167 (1987).
L. Abbott, Phys. Lett. B 150, 427 (1985).
S. Hawking, Phys. Lett. B 134, 403 (1984).
R. R. Caldwell, R. Dave, and P. J. Steinhard, Phys. Rev. Lett. 80, 1582 (1998).
T. Banks, Nucl. Phys. B 249, 332 (1985); arXiv:hepth/0305206 (2003).
S. Weinberg, Phys. Rev. Lett. 59, 2607 (1987).
V. Rubakov, Phys. Rev. D 61, 061501 (2000).
P. Steinhard and N. Turok, Science 312, 1180 (2006); arXiv:astro-ph/0605173 (2006).
A. Vilenkin, in Universe or Multiverse, Ed. by B. J. Carr and Q. Mary (Cambridge Univ. Press, Cambridge, 2007), p. 163; arXiv:astro-ph/0407586 (2004).
J. Garriga and A. Vilenkin, Progr. Theor. Phys. Suppl. 163, 245 (2006); arXiv:hep-th/0508005 (2005).
J. Polchinski, arXiv:hep-th/0603249 (2006).
A. Linde, J. Cosmol. Astropart. Phys. 0701, 022 (2007); arXiv:hep-th/0611043 (2006).
R. Bousso, R. Harnik, G. D. Kribs, and G. Perez, Phys. Rev. D 76, 043513 (2007); arXiv:hep-th/0702115 (2007).
B. Feldstein, L. Hall, and T. Watari, Phys. Rev. D 72, 123506 (2005); arXiv:hep-th/0506235 (2005).
E. Komatsu, J. Dunkley, M. R. Nolta, et al., Astrophys. J. Suppl. Ser. 180, 330 (2009); arXiv:0803.0547 [astro-ph] (2008).
M. Hicken, W. M. Wood-Vasey, S. Blondin, et al., Astrophys. J. 700, 1097 (2009).
V. Burdyuzha and G. Vereshkov, Astrophys. Space Sci. 305, 235 (2006).
A. Dolgov, arXiv:hep-ph/0405089 (2004).
V. Burdyuzha, G. Vereshkov, and J. Pacheco, arXiv:0801.0044 [gr-qc] (2008).
V. Burdyuzha, O. Lalakulich, Yu. Ponomarev, and G. Vereshkov, Phys. Rev. D 55, 7340R (1997).
E. Shuryak, Phys. Rep. 264, 357 (1996).
Ya. B. Zel’dovich, JETP Lett. 6, 316 (1967).
N. S. Kardashev, Astron. Rep. 41, 715 (1997).
V. Burdyuzha, in Particles, Strings and Cosmology (PASCOS’98), Proceedings of the 6th International Symposium, Boston, USA, 22–29 March, 1998, Ed. by P. Nath (World Scientific, Pearland, TX, 1999), p. 101.
C. Balazs and I. Szapidi, arXiv:hep-th/0603133 (2006).
W. Fischler and L. Susskind, arXiv:hep-ph/9806039 (1998).
T. Jacobson, Phys. Rev. Lett. 75, 260 (1995).
Ch. Eling, R. Guedens, and T. Jacobson, Phys. Rev. Lett. 96, 121301 (2006); arXiv:gr-qc/0602001 (2006).
G.’ t Hooft, arXiv:gr-qc/9310026 (1993).
S. Hawking, Commun.Math. Phys. 43, 199 (1975).
J. D. Bekenstein, Phys. Rev. D 7, 2333 (1973).
E. Komatsu, K. M. Smith, J. Dunkley, et al., Astrophys. J. Suppl. Ser. 192, 18 (2011); arXiv:1001.4538 [astro-ph.CO] (2010).
N. Wright, Publ. Astron. Soc. Pacif. 118, 1711 (2006).
D. A. Howell, A. Conley, M. Della Valle, et al., arXiv:0903.1086 [astro-ph.SR] (2009).
V. Burdyuzha, O. Lalakulich, Yu. Ponomarev, and G. Vereshkov, Astron. Astrophys. Trans. 23, 453 (2004).
J. M. Maldacena, Adv. Theor. Math. Phys. 2, 231 (1998).
E. Verlinde, J. High Energy Phys. 1104, 029 (2011); arXiv:1001.0785 [hep-th] (2010).
G. Wolschin, Conference Probes the Dark Side of the Universe, CERN Courier (March 2009).
R. Caldwell and M. Kamionkowski, Ann. Rev. Nucl. Part. Sci. 59, 397 (2009).
P. Serra, in Proceedings of the 45th Rencontres de Moriond, La Thuile, Italy, 2010 (in press); arXiv:1005.2415 [astro-ph.CO] (2010).
M. Jamil, Phys. Lett. B 694, 284 (2011); arXiv:1010.0385 [hep-th] (2010).
S. Dutta and R. J. Scherrer, Phys. Rev. D 82, 043526 (2010); arXiv:1004.3295 [astro-ph.CO] (2010).
M. C. March, R. Trotta, L. Amendola, and D. Huterer, Mon. Not. R. Astron. Soc. 415, 143 (2011); arXiv:1101.1521 [astro-ph.CO] (2011).
Miao Li, Xiao-Dong Li, and X. Zhang, Sci. Chin. Phys. Mech. Astron. 53, 1631 (2010); arXiv:0912.3988 [astro-ph.CO] (2009).
A. A. Starobinsky, JETP Lett. 86, 157 (2007).
E. Greewood, E. Halstead, R. Poltis, and D. Stojkovic, Phys. Rev. D 79, 103003 (2009); arXiv:0810.5343 [hep-ph] (2008).
W. Zhao, Int. J. Mod. Phys. 18, 1331 (2009); arXiv:0810.5506 [gr-qc] (2008).
A. Cooney, S. DeDeo, and D. Psaltis, Phys. Rev. D 79, 044033 (2009); arXiv:0811.3635 [astro-ph] (2008).
F. Klinkhamer and G. Volovik, Phys. Rev. D 79, 063527 (2009); arXiv:0811.4347 [gr-qc] (2008).
D. Hooper and S. Dodelson, Astropart. Phys. 27, 113 (2007); arXiv:astro-ph/0512232 (2005).
P. Zang, R. Bean, M. Liguori, and S. Dodelson, arXiv:0809.2836 [astro-ph] (2008).
A. Kempf, Phys. Rev. Lett. 103, 231301 (2009); arXiv:0908.3061 [gr-qc] (2009).
R. Banerjee and B. R. Majhi, Phys. Lett. B 69, 83 (2010); arXiv:1002.0985 [gr-qc] (2010).
J. Makela, arXiv:1001.3808 [gr-qc] (2010).
R. G. Cai, L. M. Cao, and N. Ohta, Phys. Rev. D 81, 06501 (2010); arXiv:1001.3470 [hep-th] (2010).
F. W. Shu and Y. Gong, Int. J. Mod. Phys. D 20, 553 (2011); arXiv:1001.3237 [gr-qc] (2010).
T. Padmanabhan, Gen. Relat. Gravit. 42, 2743 (2010); arXiv:1001.3380 [gr-qc] (2010).
G. F. Smoot, Int. J. Mod. Phys.D19, 2247 (2010).
A. D. Sakharov, Sov. Phys. Dokl. 12, 1040 (1967).
S. Khakshournia, Gravit. Cosmol. 16, 178 (2010).
Author information
Authors and Affiliations
Corresponding author
Additional information
Original Russian Text © V.V. Burdyuzha, 2012, published in Astronomicheskii Zhurnal, 2012, Vol. 89, No. 6, pp. 451–457.
Rights and permissions
About this article
Cite this article
Burdyuzha, V.V. The vacuum component of the Universe (cosmological constant) should evolve. Astron. Rep. 56, 403–409 (2012). https://doi.org/10.1134/S1063772912050010
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1134/S1063772912050010