Letter: Density Perturbations in a Universe Dominated by the Chaplygin Gas

Fabris, J. C.; Gonçalves, S. V. B.; Souza, Paulo Estevão de

doi:10.1023/a:1015266421750

Cited by 284 publications

(220 citation statements)

References 9 publications

Supporting

Mentioning

211

Contrasting

Unclassified

Order By: Relevance

“…Consider, for example, the Chaplygin gas cosmological model introduced in [16] and further developed in [17,18,19,20]. This model is the simplest one unifying dark matter and dark energy in a FRW background.…”

Section: Introductionmentioning

confidence: 99%

Stability properties of some perfect fluid cosmological models

et al. 2005

View full text Add to dashboard Cite

Flat FRW perfect fluid cosmologies can be reproduced as particular solutions of suitable field theoretical models. Here we investigate the stability of perfect fluid model trajectories with respect to sets of trajectories of the corresponding field models having generic initial conditions. It is shown that the trajectories of barotropic perfect fluid models and those of the Chaplygin gas model are stable. The total probability to reach the Chaplygin gas regime early enough to achieve a matter dominated stage having a realistic duration is calculated for a scalar field model assuming a natural measure in the space of initial conditions taken near a cosmological singularity. An example is presented of a two-fluid cosmological model where the stability is partially absent.

show abstract

Section: Introductionmentioning

confidence: 99%

Stability properties of some perfect fluid cosmological models

et al. 2005

View full text Add to dashboard Cite

show abstract

“…Cosmological perturbations of the GCg-fluid have been considered in [7], [9]- [16]. In [12] it was claimed that the matter power spectrum strongly constrains the parameter space of unified dark matter models, essentially ruling them out.…”

Section: Introductionmentioning

confidence: 99%

Large scale structure and the generalized Chaplygin gas as dark energy

2004

View full text Add to dashboard Cite

The growth of large scale structure is studied in a universe containing both cold dark matter (CDM) and generalized Chaplygin gas (GCg). GCg is assumed to contribute only to the background evolution of the universe while the CDM component collapses and forms structures. We present some new analytical as well as numerical results for linear and non-linear growth in such model. The model passes the standard cosmological distance test without the need of a cosmological constant (LCDM). But we find that the scenario is severely constrained by current observations of large scale structure. Any small deviations of the GCg parameters away from the standard Lambda dominated cosmology (LCDM) produces substantial suppression for the growth of structures.

show abstract

“…The negative pressure following from the Chaplygin equation of state could also be used for the description of certain effects in deformable solids [36], of stripe states in the context of the quantum Hall effect and of other phenomena. The Chaplygin gas emerges as an effective fluid associated with d-branes [37]- [38] and can also be derived from Born-Infeld type Lagrangians [32], [39]. One of its most remarkable property is that it describes a transition from a decelerated cosmological expansion to a stage of cosmic acceleration.…”

mentioning

confidence: 99%

Friedman—Robertson—Walker Models with Late-Time Acceleration

Abdussattar¹,

Prajapati²

2011

Chinese Phys. Lett.

View full text Add to dashboard Cite

In order to account for the observed cosmic acceleration, a modification of the ansatz for the variation of density in Friedman-Robertson-Walker (FRW) models given by Islam is proposed.The modified ansatz leads to an equation of state which corresponds to that of a variable Chaplygin gas, which in the course of evolution reduces to that of a modified generalized Chaplygin gas (MGCG) and a Chaplygin gas (CG), exhibiting late-time acceleration.We consider the homogeneous and isotropic Robertson-Walker space-timedescribed by its scale factor R(t) and curvature parameter k = 0, ±1. The universe is assumed to be filled with a distribution of matter represented by the energy-momentum tensor of a perfect fluid given bywhere ρ is the energy density of the cosmic matter and p is its pressure. The Einstein field equationsfor the space-time (1) yield the following two independent equations 8πGρ = 3Ṙ 2 R 2 + 3 k R 2 (4)1

show abstract

Letter: Density Perturbations in a Universe Dominated by the Chaplygin Gas

Cited by 284 publications

References 9 publications

Stability properties of some perfect fluid cosmological models

Stability properties of some perfect fluid cosmological models

Large scale structure and the generalized Chaplygin gas as dark energy

Friedman—Robertson—Walker Models with Late-Time Acceleration

Contact Info

Product

Resources

About