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Evolution of Holographic Dark Energy in Interacting Modified Chaplygin Gas Model |
WANG Cong, WU Ya-Bo, LIU Fei |
Department of Physics, Liaoning Normal University, Dalian 116029 |
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Cite this article: |
WANG Cong, WU Ya-Bo, LIU Fei 2009 Chin. Phys. Lett. 26 029801 |
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Abstract We investigate the modified Chaplygin gas (MCG) with interaction between holographic dark energy proposed by Li and dark matter. In this model, evolution of the universe is described in detail, which is from deceleration to acceleration. Specifically, the evolutions of related cosmological quantities such as density parameter, the equation of state of holographic dark energy, deceleration parameter and transition redshift are discussed. Moreover, we also give their present values which are consistent with the lately observations. Furthermore, the results given by us show such a model can accommodate a transition of the dark energy from a normal state wX>-1 to wX<-1 phantom regimes.
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Keywords:
98.80.Es
98.80.Jk
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Received: 30 July 2008
Published: 20 January 2009
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PACS: |
98.80.Es
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(Observational cosmology (including Hubble constant, distance scale, cosmological constant, early Universe, etc))
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98.80.Jk
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(Mathematical and relativistic aspects of cosmology)
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[1] Riess A G et al 1998 Astron. J. 116 1009 [arXiv:astro-ph/9805201] [2]Perlmutter S et al 1999 Astrophys. J. 517 565 [arXiv:astro-ph/9812133] [3]de Bernardis P et al 2000 Nature 404 955 [arXiv:astro-ph/0004404] [4]Hinshaw G et al 2008 arXiv:0803.0732 [astro-ph] [5]Komatsu E and Dunkley J et al 2008arXiv:0803.0547 [astro-ph] [6]Perlmutter S et al 2003 Astrophys. J. 598 102 [arXiv:astro-ph/0309368] [7]Carroll S M 2001 Living Rev. Rel. 4 1 [arXiv:astro-ph/0004075] [8]Peebles P J E and Ratra B 2003 Rev. Modern Phys. 75 559 [arXiv:astro-ph/0207347] [9]Caldwell R R, Dave R and Steinhardt P J 1998 Phys.Rev. Lett. 80 1582 [arXiv:astro-ph/9708069] [10]Peebles P J E and Ratra B 1998 Astrophys. J. 325 L17 [11]Caldwell R R 2002 Phys. Lett. B 545 23 [arXiv:astro-ph/9908168] [12]Carroll S M, Hoffman M and Trodden M 2003 Phys. Rev.D 68 023509 [arXiv:astro-ph/0301273] [13]Alam U and Sahni V 2002 [arXiv:astro-ph/0209443] [14]Kamenshchik A, Moschella U and Pasquier V 2001 Phys.Lett. B 511 265 [arXiv:gr-qc/0103004] [15]Zhu Z 2004 Astron Astrophys. 423 421 [arXiv:astro-ph/0411039] [16]Bilic N, Tupper G B and Viollier R D 2002 Phys.Lett. B 535 17 [arXiv:astro-ph/0111325] [17]Bento M C, Bertolami O and Sen A A 2002 Phys. Rev. D 66 043507 [arXiv:gr-qc/0202064] [18] Li M 2004 Phys. Lett. B 603 1 [arXiv:hep-th/0403127] [19]Huang Q G and Li M 2004 J. Cosmol. Astropart. Phys. 0408 013 { [arXiv:astro-ph/0404229] [20]Li M, Lin C S and Wang Y 2008 J. Cosmol. Astropart.Phys. 05 023 arXiv:0801.1407 [astro-ph] [21]Cohen A, Kaplan D and Nelson A 1999 Phys. Rev. Lett. 82 4971 [arXiv:hep-th/9803132] [22]Wang B, Gong Y G and Abdalla E 2005 Phys. Lett. B 624 141 [arXiv:hep-th/0506069] [23]Benaoum H B 2002 [arXiv:hep-th/0205140] [24]Chimento L P 2004 Phys. Rev. D 69 123517 [arXiv:astro-ph/0311613] [25]Chimento L P and Lazkoz R 2005 Phys. Lett. B 615 146-152 [arXiv:astro-ph/0411068] [26]Debnath U, Banerjee A and Chakraborty S 2004 Class.Quant. Grav. 21 5609 [arXiv:gr-qc/0411015] [27]Wu Y B and Li S et al 2007 Mod. Phys. Lett. A 22 783 [28]Wu Y B and Li S et al 2007 Gen. Relat. Grav. 39 653 [29]Li X Z and Liu D J 2005 Chin. Phys. Lett. 22 7 [30]Firmani C et al 2005 Mon. Not. Roy. Astron. Soc. 360 L1 [arXiv:astro-ph/0501395] |
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