Abstract
Locally rotationally symmetric Bianchi type I cosmological models are examined in the presence of dynamically anisotropic dark energy and perfect fluid. We assume that the dark energy (DE) is minimally interacting, has dynamical energy density, anisotropic equation of state parameter (EoS). The conservation of the energy-momentum tensor of the DE is assumed to consist of two separately additive conserved parts. A special law is assumed for the deviation from isotropic EoS, which is consistent with the assumption on the conservation of the energy-momentum tensor of the DE. Exact solutions of Einstein’s field equations are obtained by assuming a special law of variation for the mean Hubble parameter, which yields a constant value of the deceleration parameter. Geometrical and kinematic properties of the models and the behaviour of the anisotropy of the dark energy have been carried out. The models give dynamically anisotropic expansion history for the universe that allows to fine tune the isotropization of the Bianchi metric, hence the CMB anisotropy.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Guth A.H.: Phys. Rev. D 23, 347 (1981)
Sato K.: Mon. Notices Roy. Astron. Soc. 195, 467 (1981)
Linde A.D.: Phys. Lett. B 108, 389 (1982)
Albrecht A., Steinhardt P.J.: Phys. Rev. Lett. 48, 1220 (1982)
Parker L.: Phys. Rev. 183, 1057 (1969)
Birrell N.D., Davies P.C.W.: Quantum Fields in Curved Space. Cambridge University Press, Cambridge (1982)
Mukhanov V.F., Chibisov G.V.: Sov. Phys. J. Exper. Theor. Phys. Lett. 33, 532–535 (1981)
Hawking S.W.: Phys. Lett. B 115, 295 (1982)
Guth A.H., Pi S.Y.: Phys. Rev. Lett. 49, 1110 (1982)
Starobinsky A.A.: Phys. Lett. B 117, 175 (1982)
Bardeen J.M. et al.: Phys. Rev. D 28, 679 (1983)
Mukhanov V.F. et al.: Phys. Rep. 215, 203 (1992)
Peiris H.V. et al.: Astrophys. J. Suppl. Ser. 148, 213–231 (2003) [arXiv:astro-ph/0302225v2]
Liddle A.R., Lyth D.H.: Cosmological Inflation and Large-Scale Structure. Cambridge University Press, Cambridge (2000)
Smoot G.F. et al.: Astrophys. J. 396, L1 (1992)
Bennett C.L. et al.: Astrophys. J. 464, L1–L4 (1996) [arXiv:astro-ph/9601067]
Hinshaw G. et al.: Astrophys. J. Suppl. Ser. 148, 135 (2003) [arXiv:astro-ph/0302217v1]
Hinshaw G. et al.: Astrophys. J. Suppl. Ser. 170, 288 (2007) [arXiv:astro-ph/0603451v2]
Nolta M.R. et al.: Astrophys. J. Suppl. Ser. 180, 296–305 (2009) [arXiv:astro-ph/0803.0593]
Hinshaw G. et al.: Astrophys. J. Suppl. Ser. 180, 225–245 (2009) [arXiv:astro-ph/0803.0732]
Eriksen H.K. et al.: Astrophys. J. 605, 14–20 (2004) [arXiv:astro-ph/0307507]
Copi C.J. et al.: Mon. Notices Roy. Astron. Soc. 367, 79–102 (2006) [arXiv:astro-ph/0508047]
Spergel D.N. et al.: Astrophys. J. Suppl. Ser. 170, 377–408 (2007) [arXiv:astro-ph/0603449]
Gold B. et al.: Astrophys. J. Suppl. Ser. 180, 265–282 (2009) [arXiv:astro-ph/0803.0715]
Hill R.S. et al.: Astrophys. J. Suppl. Ser. 180, 246–264 (2009) [arXiv:astro-ph/0803.0570]
Ellis G.F.R.: Gen. Relat. Gravit. 38(6), 1003–1015 (2006)
Campanelli L. et al.: Phys. Rev. Lett. 97, 131302 (2006)
Campanelli L. et al.: Phys. Rev. D 76, 063007 (2007) [arXiv:astro-ph/0706.3802v2]
Longo, M.J.: arXiv:astro-ph:/0703325, arXiv:astro-ph:/0703694, arXiv:astro-ph:/0707.3793, arXiv: astro-ph:/0708.4013
Nodland B., Ralston J.P.: Phys. Rev. Lett. 78, 3043 (1997) [arXiv:astro-ph/9704196]
Hutsemekers D. et al.: Astron. Astrophys. 441, 915–930 (2005) [arXiv:astro-ph/0507274]
Battye R.A. et al.: Mon. Notices Roy. Astron. Soc. 385, 274–282 (2008)
Borguet B. et al.: Astron. Astrophys. 478, 321–333 (2008) [arXiv:astro-ph:/0710.4048v1]
Borguet, B., et al.: arXiv:astro-ph:/0710.4072v2
Joshi S.A. et al.: Mon. Notices Roy. Astron. Soc. 380(1), 162–174 (2007) [arXiv:astro-ph:/0705. 2548v1]
Rakic A., Schwarz D.J.: Phys. Rev. D 75, 103002 (2007) [arXiv:astro-ph/0703266v3]
Rakic, A., et al.: arXiv:astro-ph:/0609188v2
Ellis, G.F.R.: Modern Cosmology. In: Bonometto, S., et al. (ed.) Institute of Physics Publishing, Bristol, pp. 138–139 (2002)
Rodrigues D.C.: Phys. Rev. D 77, 023534 (2008) [arXiv:astro-ph/0708.1168v2]
Carroll S.M., Hoffman M.: Phys. Rev. D 68, 023509 (2003) [arXiv:astro-ph/0301273]
Nesseris S., Perivolaropoulos L.: J. Cosmol. Astropart. Phys. 0701, 018 (2007) [arxiv:astro-ph/ 0610092v3]
Riess A.G. et al.: Astrophys. J. 607, 665–687 (2004) [arXiv:astro-ph/0402512]
Astier P. et al.: Astron. Astrophys. 447, 31–48 (2006) [arXiv:astro-ph/0510447]
Komatsu E. et al.: Astrophys. J. Suppl. Ser. 180, 330–376 (2009) [arXiv:astro-ph/0803.0547]
MacTavish C.J. et al.: Astrophys. J. 647, 799 (2006) [arXiv:astro-ph/0507503v1]
Eisenstein G. et al.: Astrophys. J. 633, 560–574 (2005) [arXiv:astro-ph/0501171]
Zhao G.B. et al.: Phys. Lett. B 648, 8–13 (2007) [arXiv:astro-ph/0612728v2]
Copeland E.J. et al.: Int. J. Mod. Phys. D 15, 1753–1936 (2006) [arXiv:hep-th/0603057v3]
Koivisto T., Mota, D.F.: arXiv:astro-ph/0801.3676v2 (2008)
Koivisto T., Mota D.F.: Astrophys. J. 679, 1 (2008) [arXiv:astro-ph/0707.0279v3]
Mota D.F. et al.: Mon. Notices Roy. Astron. Soc. 382, 793–800 (2007) [arXiv:astro-ph/0708.0830v2]
Burdyuzha V., Vereshkov G.: Astrophys. Space Sci. 305, 235–239 (2006)
Turner M., Huterer D.: J. Phys. Soc. Jpn. 76, 111015 (2007) [arXiv:astro-ph/0706.2186v2]
Singh C.P., Kumar S.: Int. J. Mod. Phys. D 15, 419–438 (2006)
Kumar S., Singh C.P.: Astrophys. Space Sci. 312, 57–62 (2007)
Singh C.P.: Pramana J. Phys. 68, 707–720 (2007)
Singh C.P. et al.: Astrophys. Space Sci. 315, 181–189 (2008)
Berman M.S.: Nuovo Cimento B 74, 182–186 (1983)
Berman M.S., Gomide F.M.: Gen. Relativ. Gravit. 20, 191–198 (1988)
Author information
Authors and Affiliations
Corresponding author
Rights and permissions
About this article
Cite this article
Akarsu, Ö., Kılınç, C.B. LRS Bianchi type I models with anisotropic dark energy and constant deceleration parameter. Gen Relativ Gravit 42, 119 (2010). https://doi.org/10.1007/s10714-009-0821-y
Received:
Accepted:
Published:
DOI: https://doi.org/10.1007/s10714-009-0821-y