Bianchi type-VIo Universe with wet dark fluid
Raghavendra Chaubey
DOI: 10.4236/ns.2011.310107   PDF   HTML     3,687 Downloads   7,294 Views   Citations


The Bianchi type- VIo universe filled with dark energy from a wet dark fluid has been considered. A new equation of state for the dark energy component of the universe has been used. It is modeled on the equation of state p=γ(ρ-ρ) which can describe a liquid, for example water. The exact solutions to the corresponding field equations are obtained in quadrature form. The solution for constant deceleration parameter have been studied in detail for power-law and exponential forms both. The case γ=0, γ=1, and γ=1/3 have been also analysed.

Share and Cite:

Chaubey, R. (2011) Bianchi type-VIo Universe with wet dark fluid. Natural Science, 3, 817-826. doi: 10.4236/ns.2011.310107.

Conflicts of Interest

The authors declare no conflicts of interest.


[1] Riess, A.G. et al. (1998) Observational evidence from supernovae for an accelerating universe and cosmological constant. Astronomical Journal, 116, 1009. doi:10.1086/300499
[2] Perlmutter, S., et al. (1999) Measurements of ? and ? from 42 high-redshift supernovae. Astrophysical Journal, 517, 565. doi:10.1086/307221
[3] Sahni, V. (2004) Dark matter and dark energy. arXiv: astro-ph/0403324 (preprint), 2004.
[4] Ratra, B. and Peebles, P.J.E. (1988) Cosmological consequences of a rolling homogeneous scalar field. Physical Review D, 37, 3406. doi:10.1103/PhysRevD.37.3406
[5] Caldwell, R.R., Dave, R. and Steinhardt, P.J. (1998) Cosmological imprint of an energy component with general equation of state. Physical Review Letters, 80, 1582. doi:10.1103/PhysRevLett.80.1582
[6] Barreiro, T., Copeland, E.J. and Nunes, N.J. (2000) Quintessence Arinsing from Exponential Potentials. Phy- sical Review D, 61, 127301. doi:10.1103/PhysRevD.61.127301
[7] Armendariz-Picon, C., Damour, T. and Mukhanov, V. (2001) K-inflation. Physics Letters B, 458, 209. doi:10.1016/S0370-2693(99)00603-6
[8] Armendariz-Picon, C., Mukhanov, V. and Steinhardt, P.J. (2001) Essentials of K-essence. Physical Review D, 63, 103510. doi:10.1103/PhysRevD.63.103510
[9] Gonzalez-Diaz, P.F. (2004) K-essential phantom energy: Doomsday around the corner? Physics Letters B, 586, 1. doi:10.1016/j.physletb.2003.12.077
[10] Caldwell, R.R. (2002) A phantom menace? cosmological consequences of dark energy component with super-negative equation of state. Physics Letters B, 545, 23. doi:10.1016/S0370-2693(02)02589-3
[11] Carroll, S.M., Hoffman, M. and Trodden, M. (2003) Can the dark energy equation-of-state parameter ? be less than -1? Physical Review D, 68, 023509. doi:10.1103/PhysRevD.68.023509
[12] Elizalde, E., Nojiri, S. and Odintsov, S.D. (2004) Late-time cosmology in a (phantom) scalar-tensor theory: Dark energy and the cosmic speed up. Physical Review D, 70, 043539. doi:10.1103/PhysRevD.70.043539
[13] Freese, K. and Lewis, M. (2002) Cardassian expansion: A model in which the universe is flat, matter dominated, and accelerating. Physics Letters B, 540, 1. doi:10.1016/S0370-2693(02)02122-6
[14] Gondolo, P. and Freese, K. (2003) Fluid interpretation of cardassian expansion. Physical Review D, 68, 063509. doi:10.1103/PhysRevD.68.063509
[15] Deffayet, C., Dvali, G.R. and Gabadadze, G. (2002) Accelerated universe from gravity leaking to extra dimensions. Physical Review D, 65, 044023. doi:10.1103/PhysRevD.65.044023
[16] Dvali, G., Gabadadze, G. and Porrati, M. (2000) 4D gravity on a brane in 5D minkowski space. Physics Letters B, 485, 208. doi:10.1016/S0370-2693(00)00669-9
[17] Dvali, G. and Turner, M.S. (2003) Dark energy as a modification of the friedmann equation. arXiv: astro-ph/ 0301510.
[18] Xanthopuolos, B.C. (1987) Perfect fluids satisfying a less than extremely relativistic equation of state. Journal of Mathematical Physics, 28, 905. doi:10.1063/1.527581
[19] Gorini, V., Kamenshchik, A., Moschella, U. and Pasquier, V. (2004) The chaplygin gas as a model for dark energy. arXiv: gr-qc/0403062 (preprint).
[20] Tait, P.G. (1888) The voyage of H.M.S. challenger. London: H.M.S.O., 2, 1-73.
[21] Hayward, A.T.J. (1967) Compressibility equations for liquids: A comprative study. British Journal of Applied Physics, 18, 965. doi:10.1088/0508-3443/18/7/312
[22] Chiba, T., Sugiyama, N. and Nakamura, T. (1998) Observational tests of X-matter models. Monthly Notices of the Royal Astronomical Society, 301, 72. doi:10.1046/j.1365-8711.1998.02012.x
[23] Holman, R. and Naidu, S. (2005) Dark energy from wet dark fluid. arXiv: astro-ph/0408102 (preprint).
[24] Riess, A., et al., (2004) Type Ia supernova discoveries at z > 1 from the hubble space telescope: evidence for past deceleration and constraint on dark energy evolution. arXiv: astro-ph/0402512 (preprint).
[25] Bennett, C.L., et al., (2003) First-year Wilkinson Microwave Anisotropy Probe (WMAP) obsevations: Preliminary maps and basic results. Astrophysical Journal Supplement, 148, 1. doi:10.1086/345346
[26] Spergel, D.N. (2003) First-year Wilkinson Microwave Anisotropy Probe (WMAP) obsevations: Determination of cosmological parameters. Astrophysical Journal Supplement, 148, 175. doi:10.1086/377226
[27] Tegmark, M., Hamilton, A.J.S. and Xu, Y.Z. (2002) The power spectrum of galaxies in the 2dF 100k redshift survey. MNRAS, 335, 887. doi:10.1046/j.1365-8711.2002.05622.x
[28] Babichev, E., Dokuchaev, V. and Eroshenkos, Y. (2004) Dark energy cosmology with generalized linear equation of state. arXiv: astro-ph/0407190 (preprint).
[29] Singh, T. and Chaubey, R. (2008) Bianchi type-I universe with wet dark fluid. Pramana—Journal of Physics, 71, 447-458.
[30] Chaubey, R. (2009) Bianchi type-V universe with wet dark fluid. Astro. Phys. Space Science, 321, 241-246. doi:10.1007/s10509-009-0027-5
[31] Singh, T. and Chaubey, R. (2007) Bianchi type-V cosmological models with a viscous fluid and ? -term. Pramana—Journal of Physics, 68, 721-734.
[32] Singh, T. and Chaubey, R. “Bianchi type-V and VIo universes with dilaton and magnetic fields. International Journal of Modern Physics D, 15, 111.

Copyright © 2020 by authors and Scientific Research Publishing Inc.

Creative Commons License

This work and the related PDF file are licensed under a Creative Commons Attribution 4.0 International License.