We study cosmological application of interacting holographic dark energy density in the scalar Gauss-Bonnet framework. We employ the interacting holographic model of dark energy to obtain the equation of state for the interacting holographic energy density in a spatially flat universe. Our calculations show that taking ΩΛ=0.73 for the present time, it is possible to have wΛeff crossing -1. This implies that one can generate a phantom-like equation of state from the interacting holographic dark energy model in flat universe in the scalar Gauss-Bonnet cosmology framework. Then we reconstruct the potential of the scalar field.
Abstract：We study cosmological application of interacting holographic dark energy density in the scalar Gauss-Bonnet framework. We employ the interacting holographic model of dark energy to obtain the equation of state for the interacting holographic energy density in a spatially flat universe. Our calculations show that taking ΩΛ=0.73 for the present time, it is possible to have wΛeff crossing -1. This implies that one can generate a phantom-like equation of state from the interacting holographic dark energy model in flat universe in the scalar Gauss-Bonnet cosmology framework. Then we reconstruct the potential of the scalar field.
M. R. Setare. Interacting Holographic Dark Energy in the Scalar Gauss-Bonnet Gravity[J]. 中国物理快报, 2009, 26(2): 29501-029501.
M. R. Setare. Interacting Holographic Dark Energy in the Scalar Gauss-Bonnet Gravity. Chin. Phys. Lett., 2009, 26(2): 29501-029501.
[1] Riess A G et al 1998 Astron. J. 116 1009 Perlmutter S et al 1999 Astrophys. J. 517 565 Astier P et al 2006 Astron. Astrophys. 447 31 [2] Tegmark M et al 2004 Phys. Rev. D 69 103501 Abazajian K et al 2004 Astron. J. 128 502 Abazajian K et al 2005 Astron. J. 129 1755 [3] Spergel D N et al 2003 Astrophys. J. Suppl. 148 175 Spergel D N et al astro-ph/0603449 [4] Kachru S, Kallosh R, Linde A and Trivedi S P 2003 Phys. Rev. D 68 046005 [5] Susskind L hep-th/0302219 [6] Cohen A G, Kaplan D B and Nelson A E 1999 Phys. Rev.Lett. 82 4971 [7] Horava P and Minic D 2000 Phys. Rev. Lett. 851610 Thomas S D, 2002 Phys. Rev. Lett. 89 081301 [8] Hsu S D H 2004 Phys. Lett. B 594 13 [9] Li M 2004 Phys. Lett. B 603 1 [10] 't Hooft G gr-qc/9310026 Susskind L 1995 J. Math. Phys. 36 6377 [11] Huang Q G and Gong Y G 2004 J. Cosmol. Astropart.Phys. 0408 006 Enqvist K, Hannestad S and Sloth M S 2005 J. Cosmol.Astropart. Phys. 0502 004 Shen J, Wang B, Abdalla E and Su R K 2005 Phys. Lett. B 609 200 Kao H C, Lee W L and Lin F L 2005 Phys. Rev. D 71123518 [12] Huang Q G and Li M 2004 J. Cosmol. Astropart. Phys. 0408 013 Enqvist K and Sloth M S 2004 Phys. Rev. Lett. 93221302 Ke K and Li M 2005 Phys. Lett. B 606 173 Huang Q G and Li M 2005 J. Cosmol. Astropart. Phys. 0503 001 Pavon D and Zimdahl W 2005 Phys. Lett. B 628 206 Wang B, Gong Y and Abdalla E 2005 Phys. Lett. B 624 141 Nojiri S and Odintsov S D 2006 Gen. Rel. Grav. 381285 Elizalde E , Nojiri S, Odintsov S D and Wang P 2005 Phys. Rev. D 71 103504 Hu B and Ling Y 2006 Phys. Rev. D 73 123510 Li H, Guo Z K and Zhang Y Z 2006 Int. J. Mod. Phys. D 15 869 Setare M R , Zhang J, Zhang X 2007 J. Cosmol.Astropart. Phys. 0703 007 Setare M R 2007 Phys. Lett. B 648 329 [13] Amendola L and Tocchini-Valentini D 2001 Phys. Rev.D 64 043509 Zimdahl W, Schwarz D J, Balakin A B and Pavon D 2001 Phys. Rev. D 64 063501 Balakin A B, Pavon D, Schwarz D J and Zimdahl W 2003 NewJ. Phys. 5 085 Horvat R 2004 Phys. Rev. D 70 087301 Wang P and Meng X H 2005 Class. Quant. Grav. 22283 Wang B,Lin C Y and Abdalla E 2006 Phys. Lett. B 637 357 Berger M S and Shojaei H 2006 Phys. Rev. D 73083528 Setare M R 2007 Eur. Phys. J. C 50 991 Setare M R 2007 J. Cosmol. Astropart. Phys. 0701023 Setare M R 2007 Phys. Lett. B 654 1 [14] Gong Y 2004 Phys. Rev. D 70 064029 [15] Kim H, Lee H W, and Myung Y S 2005 Phys. Lett. B 628 11 [16] Torres D F 2002 Phys. Rev. D 66 043522 [17] Setare M R 2007 Phys. Lett. B 644 99 [18] Brans C and Dicke C H 1961 Phys. Rev. 124 925 [19] Capozziello S 2002 Int. J. Mod. Phys. D 11483 Capozziello S, Carloni S and Troisi A, arXiv:astro-ph/0303041 Carroll S M, Duvvuri V, Trodden M and Turner S 2004 Phys. Rev. D 70 043528 [20] Nojiri S and Odintsov S D 2003 Phys. Rev. D 68 123512 [21] Nojiri S, Odintsov S D and Sasaki M 2005 Phys. Rev.D 71 123509 Carter B M N, Neupane I P 2006 Phys. Lett. B 63894 Carter B M N, Neupane I P 2006 J. Cosmol. Astropart.Phys. 06 004 [22] Amendola L, Charmousis Ch and Davis S C arXiv:0704.0175 [astro-ph] [23] Koivisto T, Mota D F 2007 Phys. Lett. B 644104 Koivisto T, Mota D F 2007 Phys. Rev. D 75 023518 [24] Pavon D and Zimdahl W hep-th/0511053 [25] Kim H,Lee H W and Myung Y S 2006 Phys. Lett. B 632 605 [26] Huang Q G, Gong Y 2004 J. Cosmol. Astropart. Phys. 0408 006 [27] Kao H C, Lee W L and Lin F L astro-ph/0501487 [28] Shen J, Wang B, Abdalla E and Su R K hep-th/0412227 [29] Setare M R 2006 Phys. Lett. B 642 1 Setare M R 2006 Phys. Lett. B 642 421 [30] Nojiri S, Odintsov S D and Sami M 2006 Phys. Rev. D 74 046004 [31] Nojiri S and Odintsov S D 2007 Int. J. Geom. Meth.Mod. Phys. 4 115 Cognola G, Elizalde E Nojiri S, Odintsov S D and Zerbini S2007 Phys. Rev. D 75 086002 Nojiri S, Odintsov S D and Tretyakov P 2007 Phys. Lett.B 651 224
2009, Vol. 26 
