R. Chaubey / Natural Science 3 (2011) 817-826

Copyright © 2011 SciRes. OPEN ACCESS

826

=1q (4.50)

The model has no singularity.

5. CONCLUSIONS

The Bianchi type-VIo universe has been considered

for a new equation of state for the Dark Energy compo-

nent of the universe (known as dark wet fluid). The solu-

tion has been obtained in quadrature form. The models

with constant deceleration parameter have been dis-

cussed in detail. The behaviour of the models for large

time have been analyzed.

REFERENCES

[1] Riess, A.G., et al. (1998) Observational evidence from

supernovae for an accelerating universe and cosmologi-

cal constant. Astronomical Journal, 116, 1009.

doi:10.1086/300499

[2] Perlmutter, S., et al. (1999) Measurements of Ω 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).

[4] Ratra, B. and Peebles, P.J.E. (1988) Cosmological con-

sequences of a rolling homogeneous scalar field. Physi-

cal 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 gen-

eral 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 su-

per-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) Ac-

celerated universe from gravity leaking to extra dimen-

sions. Physical Review D, 65, 044023.

doi:10.1103/PhysRevD.65.044023

[16] Dvali, G., Gabadadze, G. and Porrati, M. (2000) 4D grav-

ity 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. Lon-

don: 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) Ob-

servational 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 Micro-

wave Anisotropy Probe (WMAP) obsevations: Prelimi-

nary maps and basic results. Astrophysical Journal Sup-

plement, 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 Sup-

plement, 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 2 dF 100 k 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. Astrophysics and Space Science, 321, 241-246.

doi:10.1007/s10509-009-0027-5

[31] Singh, T. and Chaubey, R. (2007) Bianchi type-V cos-

mological models with a viscous fluid and -term.

Pramana—Journal of Physics, 68, 721-734.

[32] Singh, T. and Chaubey, R. (1998) Bianchi type-V and

VIo universes with dilaton and magnetic fields. Interna-

tional Journal of Modern Physics D, 15, 111.