2005/01/31 by Hao Wei, Rong-Gen Cai, Ding-Fang Zeng · 11 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Dark energy #Imaging phantom #Pulsars and Gravitational Waves Research #Quantum and Classical Electrodynamics #Scalar (mathematics) #Scalar field #Scalar field dark matter #Scalar potential #astro-ph #gr-qc #hep-ph #hep-th
paper · pdf · doi:10.1088/0264-9381/22/16/005
published as Class.Quant.Grav.22:3189-3202,2005 · Latex2e, 12 pages, no figure; v2: discussions and references added, 14 pages, 3 eps figures; v3: published version
arxiv created 2005/07/22 · openalex publication_date 2005/07/22 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
Recently a lot of attention has been given to building a dark energy model in which the equation-of-state parameter w can cross the phantom divide w = −1. One of the models to realize crossing the phantom divide is called the quintom model, in which two real scalar fields appear, one is a normal scalar field and the other is a phantom-type scalar field. In this paper we propose a non-canonical complex scalar field as the dark energy, which we dub ‘hessence’, to implement crossing the phantom divide, in a similar sense as the quintom dark energy model. In the hessence model, the dark energy is described by a single field with an internal degree of freedom rather than two independent real scalar fields. However, the hessence is different from an ordinary complex scalar field, we show that the hessence can avoid the difficulty of the Q -ball formation which gives trouble to the spintessence model (an ordinary complex scalar field acts as the dark energy). Furthermore, we find that, by choosing a proper potential, the hessence could correspond to a Chaplygin gas at late times.