The Equivalence between Different Dark (Matter) Energy Scenarios

Abstract

We have shown that the phenomenological models with a cosmological constant of the type $\Lambda =\beta (\frac{\ddot{R}}{R})$ and $\Lambda =3\alpha H^2$, where $R$ is the scale factor of the universe and $H$ is the Hubble constant, are equivalent to a quintessence model with a scalar ($\varphi$) potential of the form $V\propto {\varphi }^{-n},n$ = constant. The equation of state of the cosmic fluid is described by these parameters ($\alpha ,\beta ,n$) only. The equation of state of the cosmic fluid (dark energy) can be determined by any of these parameters. The actual amount of dark energy will define the equation of state of the cosmic fluid. All of the three forms can give rise to cosmic acceleration depending the amount of dark energy in the universe.

References in corpus (3)

• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Discovery of a Supernova Explosion at Half the Age of the Universe and its Cosmological Implications
• Cosmic Acceleration With A Positive Cosmological Constant

Cited by in corpus (10)

• Can vacuum decay in our Universe?
• FRW Cosmology with Variable G and Lambda
• Gravitational Baryogenesis in Running Vacuum models
• Variable cosmological term $\Lambda (t)$
• A flat FRW model with dynamical $\Lambda$ as function of matter and geometry
• A Dark Energy Model in Kaluza-Klein Cosmology
• Astrophysics in 2005
• Generalized phenomenological models of dark energy
• Effect of Dynamical Cosmological Constant in presence of Modified Chaplygin Gas for Accelerating Universe
• Cosmological volume acceleration in dust epoch: using scaling solutions and variable cosmological term $\Lambda (t)$ within an anisotropic cosmological model