Abstract
We show that a phenomenological form of energy density for the scalar field can provide the required transition from decelerated (q > 0) to accelerated expansion (q < 0) phase of the universe. We have used the latest type Ia supernova (SNIa) and Hubble parameter datasets to constrain the model parameters. The best fit values obtained from those datasets are then applied to reconstruct ωϕ(z), the equation of state parameter for the scalar field. The results show that the reconstructed forms of q(z) and ωϕ(z) do not differ much from the standard ΛCDM value at the current epoch. Finally, the functional form of the relevant potential V(ϕ) is derived by a parametric reconstruction. The corresponding V(ϕ) comes out to be a double exponential potential, which has a number of cosmological implications. Additionally, we have also studied the effect of this particular scalar field dark energy sector on the evolution of matter overdensities.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
