Emerging the dark sector from thermodynamics of cosmological systems with constant pressure
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Cosmological constant
Quintessence
In the context of the induced matter theory of gravity, we investigate the possibility of deriving a 4D quintessential scenario where an interaction between dark energy and dark matter is allowed, and the dark energy component is modeled by a minimally coupled scalar field. Regarding the Ponce de Leon metric, we found that it is possible to obtain such scenario on which the energy densities of dark matter and dark energy, are both depending of the fifth extra coordinate. We obtain that the 4D induced scalar potential for the quintessence scalar field, has the same algebraic form to the one found by Zimdahl and Pavon in the context of usual 4D cosmology.
Quintessence
Cold dark matter
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Using cosmic voids to probe the growth rate of cosmic structure, and hence the nature of dark energy, is particularly interesting in the context of modified gravity theories that rely on the ``screening mechanism.'' In this work we improve the modelling of redshift-space distortions around voids in the dark matter density field, and thus reduce systematic errors in the derivation of cosmological parameters. We also show how specific types of voids can be used to better probe the growth rate, using a flexible void finder. We apply our results to test for a ``quintessence'' type of dark energy vs. a $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model, and find a good agreement with the fiducial cosmology after implementing an analytical correction to the radial velocity profiles around voids. We additionally outline characteristic imprints of dark energy in the dark matter velocity distributions around voids.
Quintessence
Void (composites)
Cold dark matter
Structure formation
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Quintessence
Cosmological constant
Chaplygin gas
Cold dark matter
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In this talk we present a model of the universe in which dark energy is modelled explicitely with both a dynamical quintessence field and a cosmological constant. Our results confirm the possibility of a collapsing universe (for a given region of the parameter space), which is advantageous for an adequate formulation of both perturbative quantum field and string theories. We have also reproduced the measurements of modulus distance from supernovae with good accuracy.
Quintessence
Cosmological constant
Constant (computer programming)
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We consider the fractal Friedmann-Robertson-Walker universe filled with dark fluid. By making use of this assumption, we discuss two types of dark energy models: Generalized Ricci and generalized holographic dark energies. We calculate the equation of state parameters, investigate some special limits of the results and discuss the physical implications via graphs. Also, we reconstruct the potential and the dynamics of the quintessence and k-essence(kinetic-quintessence) according to the results obtained for the fractal dark energy.
Quintessence
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The cosmological model with an interaction between dynamical quintessence dark energy and cold dark matter is considered. Evolution of a dark energy equation of state parameter is defined by a dark energy adiabatic sound speed and a dark sector interaction parameter, which must be more physically correct model then a previously used in which such evolution was given by some fixed dependence on scale factor. The constraints on interaction parameter and other parameters of the model was obtained using a cosmic microwave background, baryon acoustic oscillations and supernova SN Ia data.
Quintessence
Baryon Acoustic Oscillations
Scale factor (cosmology)
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Quintessence
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We explore unification of dark matter and dark energy in a theory containing a scalar field of non-Lagrangian type, obtained by direct insertion of a kinetic term into the energy-momentum tensor. This scalar is different from quintessence, having an equation of state between $\ensuremath{-}1$ and 0 and a zero sound speed in its rest frame. We solve the equations of motion for an exponential potential via a rewriting as an autonomous system, and demonstrate the observational viability of the scenario, for sufficiently small exponential potential parameter $\ensuremath{\lambda}$, by comparison to a compilation of kinematical cosmological data.
Quintessence
Kinetic term
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We study evolution of perturbations in dark matter and dark energy for spherical collapse. We study Tachyon models of dark energy using the approach outlined in Rajvanshi and Bagla (2018). We work with models that are allowed by current observations. We find that as with Quintessence models allowed by observations, dark energy perturbations do not affect evolution of perturbations in dark matter in a significant manner. Perturbations in dark energy remain small for such models. In order to compare different classes of dark energy models, we use reconstruction of potentials and study dark matter and dark energy perturbations for same expansion history in the two models. We find that dark matter perturbations carry no imprint of the class of dark energy models for the same expansion history: this is significant in that we can work with any convenient model to study clustering of dark matter. We find that the evolution of dark energy perturbations carries an imprint of the class of models in that these grow differently in Tachyon models and Quintessence models. However, the difference between these diminishes for (1+w)<<1 and hence prospects for differentiating between models using characteristics of perturbations are limited in our Universe.
Quintessence
Tachyon
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