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Unless some unknown symmetry in Nature prevents or suppresses a non-minimal coupling in the dark sector, the dark energy field may interact with the pressureless component of dark matter.
S.M. Carroll, Phys. Rev. Lett. 81
1998
Earlier work this paper cites.
J. M. F. Maia and J. A. S. Lima, Phys. Rev. D 65
2002
Earlier work this paper cites.
A. A. Sen and S. Sethi, Phys. Lett. B 532
2002
Earlier work this paper cites.
J. S. Alcaniz and J. M. F. Maia, Phys. Rev. D 67
2003
Earlier work this paper cites.
L. Jarv, T. Mohaupt and F. Saueressig, JCAP 0408
2004
Earlier work this paper cites.
P. Wang and X. Meng, Class. Quant. Grav. 22
2005
Earlier work this paper cites.
J. S. Alcaniz and J. A. S. Lima, Phys. Rev. D 72
2005
Earlier work this paper cites.
D. J. Eisenstein et al
2005
Earlier work this paper cites.
J. Simon, L. Verde and R. Jimenez, Phys. Rev. D 71
2005
Cited alongside, same era.
M. O ¨ \ddot{\rm{O}} zer and M. O. Taha, Phys. Lett. B 171
2006
Cited alongside, same era.
P. Astier et al
2006
Cited alongside, same era.
W. J. Percival et al
2007
Cited alongside, same era.
D. N. Spergel et al
2007
Cited alongside, same era.
G. Steigman, Ann. Rev. Nucl. Part. Sci, 57
2007
Cited alongside, same era.
M. Doran, S. Stern and E. Thommes, JCAP 0704
2007
Cited alongside, same era.
I. Waga, Astrophys. J. 414
2008
Later among the works it cites.
S. Carneiro et al
2008
Later among the works it cites.
F. E. M. Costa, J. S. Alcaniz and J. M. F. Maia, Phys. Rev. D 77
2008
Later among the works it cites.
J. F. Jesus et al
2008
Later among the works it cites.
T. Padmanabhan and T.R. Choudhury, MNRAS 344
2008
Later among the works it cites.
F. E. M. Costa and J. S. Alcaniz, in preparation (2009)
2009
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S. H. Pereira and J. F. Jesus, Phys. Rev. D 79
2009
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2008
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Double exponential potentials of the type ( 10
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As discussed in Ref. [ 24 ] , the BAO parameter 𝒜 = D V Ω m H 0 2 / z c {\cal{A}}=D_{V}\sqrt{\Omega_{m}H_{0}^{2}}/zc can be considered as a good approximation for a large class of dark energy models. In our analysis, we do not use this quantity because it also uses the approximation that the sound travel distance is ∝ 1 / Ω m \propto 1/\sqrt{\Omega_{m}} , which fails if dark energy has a significant contribution in the past. According to Fig. (1a), in our interacting scenarios it may happen for relatively large and positive values of ϵ \epsilon (see [ 6 ] for a discussion)
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Note that the thermodynamical constraint ϵ > 0 \epsilon>0 seems not to apply to a general quintessence case ( w ≠ 1 w\neq 1 ). See, e.g., Refs. [ 26 ] and [ 27 ] for a discussion
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D. Pavon and B. Wang, Gen. Rel. Grav. 41
2009
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