Holographic Dark Energy Cosmological Model in Scalar Tensor Theory of Gravitation

Download PDF (167.6 KB) PP. 49 - 55 Pub. Date: September 12, 2017

DOI: 10.22606/nhmp.2017.12003

Author(s)

V.G.Mete^*
Department of Mathematics, R.D.I.K. & K.D. College, Badnera-Amravati, India.
V.D.Elkar
Department of Mathematics, J.D.Patil Sangludkar Mahavidyalaya, Daryapur, Dist.Amravati
Poonam P. Kadu
Department of Mathematics, J.D.Patil Sangludkar Mahavidyalaya, Daryapur, Dist.Amravati

Abstract

An attempt has been taken to study the minimally interacting fields, dark matter and holographic dark energy in scalar tensor theory formulated by Saez and Ballester. The exact solution of the field equations is obtained by using the fact that the scalar expansion of the universe is proportional to the shear scalar. Some physical and geometrical aspects of the model are also discussed.

Keywords

Bianchi type VIo universe, scalar- tensor theory, holographic dark energy.

References

[1] A. G. Riess et al., Astron. J. 116, 1009(astro-ph/9805201), 1998.

[2] S. Perlmutter et al., Astrophys. J. 517, 5 (astro-ph/9812133), 1999.

[3] C.L. Bennet et al., Astrophys. J. Suppl. Ser. 148, 1, 2003.

[4] M. Tegmark et al., (SDSS collaboration) Astrophys. J. Suppl. 69, 103501, 2004.

[5] S.W. Allenet al., Mon. Not. R. Astron Soc. 353, 457, 2007.

[6] R. Cadwell, R. Dave andP.J. Steinhardt, Phys. Rev.Lett. 80, 1582, 1998.

[7] A.R. Liddel and R.J.Scherrer, Phys. Rev.D59.023509, 1999.

[8] P.J. Steinhardt, L. Wang and I. Zlatev, Phys.Rev.D59, 123504, 1999.

[9] G.R., Dvali, G. Gabadadze and M. Porrati,M., Phys. Lett. B 484, 112, 2000.

[10] C. Deffayet, Phys. Lett. B 502, 199, 2001.

[11] S. Capozziello, Carloni and A.Troisi, arXiv: astro-ph/0303041, 2003.

[12] S.M. Carrol, et al., Phys. Rev. D 70, 043528, 2003.

[13] S. Nojiri and S.D.Odintsov, Phys.Rev.D 68, 123512, 2003.

[14] C.H. Brans and R. H. Dicke, Phys. Rev.124156, 925 157 6,1961.

[15] K. Nordtvedt, Post-Newtonian Metric for a General Class of Scalar-Tensor Gravitational Theories and Observational Consequences.; Ap. J. 161163, 1059, 1970.

[16] D. Saez and V.J.Ballester, Phys. Lett.A 113168, 467, 1985.

[17] T. Singh and A.K.Agrawal, Astrophys.Space Sci. 182, 289, 1991.

[18] Shri Ram and S.K.Tiwari, Astrophys.Space Sci. 277, 461, 170, 1998.

[19] K.S.Adhav, A.S. Nimkar and R.L. Naidu, Astrophys, Space Sci, 312, 165-169, 2007.

[20] L.Susskind, J.Math.Phys.36, 6377, 1995.

[21] M.Li, Phys.Lett.B, 603, 1, 2004.

[22] S. Sarkar and C.R.Mahanta, Int.J.Theor.Phys. 52, 1482, 2013.

[23] S. Sarkar, Astrophys. Space Sci. 349, 985, 2014.

[24] M.R.Setare, Phs.Lett. B, 644, 99, 2007.

[25] S. Sarkar, Astrophysics and Space Science, 349(2), 985, 2014.

[26] S. Sarkar, Astrophysics and Space Science,DOI10.1007/s10509-014-1920-0, 2014.

[27] S.Sarkar, Astrophysics and Space Science: 350(2), 821, 2014.

[28] M.R.Setare and E.C.Vanegas, Int.J.Mod.Phys.D18, 147, 2009.

[29] M.Kiran et al., Astrophys.Space Sci. DOI 10.1007/s10509-014-2099-o.

[30] K.S. Adhav, V.B.Raut and D.K. Joshi,Eur.J.Sci. and Tech 3,9, 2014.

[31] D.R.K. Reddy and V.D. Elkar,Prespacetime J. 6,4 295-304, 2015.

[32] V.U.M. Rao and U.Y.Divya Prasanthi, The African Reviews of Physics, 11, 001, 2016.

[33] B.Collins et al., Gen. Relativ.Gravit. 12, 805, 1980.

New Horizons in Mathematical Physics