Cosmological evolution of interacting dark energy in Lorentz violation

Freddy P. Zen; Bobby E. Gunara; A. Purwanto

doi:10.1140/epjc/s10052-009-1104-1

2022 Impact factor 4.4

Particles and Fields

Eur. Phys. J. C (2009) 63: 477-490
https://doi.org/10.1140/epjc/s10052-009-1104-1

Regular Article - Theoretical Physics

Cosmological evolution of interacting dark energy in Lorentz violation

Freddy P. Zen¹^,2, Arianto¹^,2^,3^*, Bobby E. Gunara¹^,2, Triyanta¹^,2 and A. Purwanto²^,4

¹ Theoretical Physics Lab., THEPI Devision, Jl. Ganesha 10, Bandung, 40132, Indonesia
² Indonesia Center for Theoretical and Mathematical Physics (ICTMP), Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Jl. Ganesha 10, Bandung, 40132, Indonesia
³ Department of Physics, Udayana University, Jl. Kampus Bukit, Jimbaran, Kuta-Bali, 80361, Indonesia
⁴ Department of Physics, Institut Teknologi Sepuluh November, Jl. Kampus Sukolilo, Surabaya, 60111, Indonesia

^* e-mail: arianto@upi.edu

Received: 8 April 2009
Revised: 15 June 2009
Published online: 31 July 2009

Abstract

The cosmological evolution of an interacting scalar-field model in which the scalar field interacts with dark matter, radiation, and baryons via Lorentz violation is investigated. We propose a model of interaction through the effective coupling, . Using dynamical system analysis, we study the linear dynamics of an interacting model and show that the dynamics of critical points are completely controlled by two parameters. Some results can be mentioned as follows. Firstly, the sequence of radiation, the dark matter, and the scalar-field dark energy exist and baryons are subdominant. Secondly, the model also allows for the possibility of having a universe in the phantom phase with constant potential. Thirdly, the effective gravitational constant varies with respect to time through . In particular, we consider the simple case where has a quadratic form and has a good agreement with the modified ΛCDM and quintessence models. Finally, we also calculate the first post-Newtonian parameters for our model.