Cosmological evolution of "hessence" dark energy and avoidance of the big rip
138 citations recorded by the source corpus.
Recently, many dark energy models whose equation-of-state parameter can cross the phantom divide w(de)=-1 have been proposed. In a previous paper [H. Wei, R. G. Cai, and D. F. Zeng, Classical Quantum Gravity 22, 3189 (2005)], we suggest such a model named hessence, in which a noncanonical complex scalar field plays the role of dark energy. In this work, the cosmological evolution of the hessence dark energy is investigated. We consider two cases: one is the hessence field with an exponential potential, and the other is with a (inverse) power-law potential. We separately investigate the dynamical system with four different interaction forms between hessence and background perfect fluid. It is found that the big rip never appears in the hessence model, even in the most general case, beyond particular potentials and interaction forms.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/9c45aeb09a7bc654c5c0fed9098c1c689ee33ce7
Citations in the corpus
- Dynamical systems applied to cosmology: Dark energy and modified gravity (2017, unknown): “Saridakis & Weller (2010) introduced the coupling ∂µφ∂ µσ, while Wei & Cai (2005) and Alimohammadi & Mohseni Sadjadi (2006) analysed the so-called hessence dark energy scenario with the Lagrangian L = −∂φ2/2 + φ2∂σ2/2− V (φ).”