New interaction between dark energy and dark matter changes sign during cosmological evolution

Sun, Cheng-Yi; Yue, Rui-Hong

doi:10.1103/physrevd.85.043010

Cited by 35 publications

(27 citation statements)

References 81 publications

(73 reference statements)

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“…Among other things, we can analyze if the density parameter of dark energy at early times (EDE) respects the constraints arising from the baryogenesis; if the redshift of sign change z Q is consistent with the results of Cai et al and if the magnitude of the ratio r in the final stage of the universe alleviates the coincidence problem and to what extent it does. A variety of interactions, which can change its sign, has been proposed [49][50][51][52]. The Wei's work matches z Q with the transition redshift to an accelerated universe z acc , while Sun et al linking z Q with a redshift for which the dark ratio r equals the inverse of the coupling constant (really there, only the case r = 1 is considered).…”

Section: The Modelsmentioning

confidence: 96%

“…In light of these considerations, among the various possible interactive proposals, Cai's work indicates that should be selected those which can change its sign along cosmological evolution. There are a few papers [49][50][51][52], where the proposals are explicit but analytical solutions are obtained only in some cases. In this paper we propose an extension of these works, considering interactions where the deceleration parameter and the interaction do not change their signs together but with a short time delay and also, a baryonic component that is not coupled to dark sector is added.…”

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confidence: 98%

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On extended sign-changeable interactions in the dark sector

Forte

2014

Gen Relativ Gravit

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We extend the cosmological couplings proposed in Sun et al. and Wei, where they suggested interactions with change of signs along the cosmological evolution. Our extension liberates the changes of sign of the interaction from the deceleration parameter and from the relation of energy densities of the dark sector and considers the presence of non interactive matter. In three cases we obtain the general solutions and the results obtained in models fitted with Hubble's function and SNe Ia data, are analyzed regarding the problem of the cosmological coincidence, the problem of the crisis of the cosmological age and the magnitude of the energy density of dark energy at early universe. Also we graphically study the range of variation of, the actual dark matter density parameter, the effective equation of state of the dark energy and the redshift of transition to the accelerated regimen, generated by variations at order $1\sigma$ in the coupling parameters.Comment: 20 pages, 26 figures,title shortened, new references added, to be published in General Relativity and Gravitation journal. The final publication will be available at Springer via link.springer.com/article/10.1007/s10714-014-1811-

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Section: The Modelsmentioning

confidence: 96%

mentioning

confidence: 98%

On extended sign-changeable interactions in the dark sector

Forte

2014

Gen Relativ Gravit

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“…Now we draw graphs between the EoS parameter w de with the parameter u in the equation (18) for three different values of interacting parameter γ 2 = 0, 0.5, 1 which is shown in (9) and (16), becomesρ…”

Section: Event Horizonmentioning

confidence: 99%

“…represents the interaction term between CDM and DE [18], γ being a constant which represents the interaction parameter. Now we present fractional energy densities as…”

Section: Frw Universe and Ecpde In Logarithmic Correction And Power Lmentioning

confidence: 99%

Study of Entropy-corrected Logarithmic and Power-law Versions of Pilgrim Dark Energy

Saha

Debnath

2015

Int J Theor Phys

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In the present work, first, we have described pilgrim dark energy, entropycorrected pilgrim dark energy for logarithmic and power law versions. Secondly, we have done the work on the aforementioned entropy-corrected versions by choosing an interacting framework with cold dark matter and three cutoffs such as Hubble, event and conformal age of the universe. We have also made the analysis of w de − w de and point out freezing region and thawing region in that plane.

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“…This gives a clue to the proposal of most general form of interaction. This is why, Sun and Yue (2012) to proposed new form of interaction term as follows…”

Section: Equation Of State Parametermentioning

confidence: 99%

Analysis of generalized ghost version of pilgrim dark energy

Sharif

Jawad

2014

Astrophys Space Sci

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The proposal of pilgrim dark energy is based on the speculation that phantom-like dark energy possesses enough resistive force to preclude the black hole formation in the later universe. We explore this phenomenon by assuming the generalized ghost version of pilgrim dark energy. We find that most of the values of the interacting (ξ 2 ) as well as pilgrim dark energy (u) parameters push the equation of state parameter towards phantom region. The squared speed of sound shows that this model remains stable in most of the cases of ξ 2 and u. We also develop ω Λ − ω ′ Λ plane and observe that this model corresponds to thawing as well as freezing regions. Finally, it is shown that the non-interacting and interacting generalized ghost versions of pilgrim dark energy correspond to ΛCDM limit on the statefinder plane.

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New interaction between dark energy and dark matter changes sign during cosmological evolution

Cited by 35 publications

References 81 publications

On extended sign-changeable interactions in the dark sector

On extended sign-changeable interactions in the dark sector

Study of Entropy-corrected Logarithmic and Power-law Versions of Pilgrim Dark Energy

Analysis of generalized ghost version of pilgrim dark energy

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