Fate of the phantom dark energy universe in semiclassical gravity. II. Scalar phantom fields

Jaume De Haro; Jaume Amoros; Emilio Elizalde

doi:10.1103/PhysRevD.86.083528

Fate of the phantom dark energy universe in semiclassical gravity. II. Scalar phantom fields

Jaume De Haro, Jaume Amoros, Emilio Elizalde

Research output: Contribution to journal › Article › Research › peer-review

5 Citations (Scopus)

Abstract

Quantum corrections coming from massless fields conformally coupled with gravity are studied, in order to see if they can lead to avoidance of the annoying big rip singularity which shows up in a flat Friedmann-Robertson-Walker universe filled with dark energy and modeled by a scalar phantom field. The dynamics of the model are discussed for all values of the two parameters, named α>0 and β<0, corresponding to the regularization process. The new results are compared with the ones obtained in previously, where dark energy was modeled by means of a phantom fluid with equation of state P=ωρ, with ω<-1. © 2012 American Physical Society.

Original language	English
Article number	083528
Journal	Physical Review D - Particles, Fields, Gravitation and Cosmology
Volume	86
Issue number	8
DOIs	https://doi.org/10.1103/PhysRevD.86.083528
Publication status	Published - 16 Oct 2012

Access to Document

10.1103/PhysRevD.86.083528

Fingerprint Dive into the research topics of 'Fate of the phantom dark energy universe in semiclassical gravity. II. Scalar phantom fields'. Together they form a unique fingerprint.

Cite this

@article{f83aaa185d234bfbbec30dd39cb537a3,

title = "Fate of the phantom dark energy universe in semiclassical gravity. II. Scalar phantom fields",

abstract = "Quantum corrections coming from massless fields conformally coupled with gravity are studied, in order to see if they can lead to avoidance of the annoying big rip singularity which shows up in a flat Friedmann-Robertson-Walker universe filled with dark energy and modeled by a scalar phantom field. The dynamics of the model are discussed for all values of the two parameters, named α>0 and β<0, corresponding to the regularization process. The new results are compared with the ones obtained in previously, where dark energy was modeled by means of a phantom fluid with equation of state P=ωρ, with ω<-1. {\textcopyright} 2012 American Physical Society.",

author = "{De Haro}, Jaume and Jaume Amoros and Emilio Elizalde",

year = "2012",

month = oct,

day = "16",

doi = "10.1103/PhysRevD.86.083528",

language = "English",

volume = "86",

number = "8",

}

TY - JOUR

T1 - Fate of the phantom dark energy universe in semiclassical gravity. II. Scalar phantom fields

AU - De Haro, Jaume

AU - Amoros, Jaume

AU - Elizalde, Emilio

PY - 2012/10/16

Y1 - 2012/10/16

N2 - Quantum corrections coming from massless fields conformally coupled with gravity are studied, in order to see if they can lead to avoidance of the annoying big rip singularity which shows up in a flat Friedmann-Robertson-Walker universe filled with dark energy and modeled by a scalar phantom field. The dynamics of the model are discussed for all values of the two parameters, named α>0 and β<0, corresponding to the regularization process. The new results are compared with the ones obtained in previously, where dark energy was modeled by means of a phantom fluid with equation of state P=ωρ, with ω<-1. © 2012 American Physical Society.

AB - Quantum corrections coming from massless fields conformally coupled with gravity are studied, in order to see if they can lead to avoidance of the annoying big rip singularity which shows up in a flat Friedmann-Robertson-Walker universe filled with dark energy and modeled by a scalar phantom field. The dynamics of the model are discussed for all values of the two parameters, named α>0 and β<0, corresponding to the regularization process. The new results are compared with the ones obtained in previously, where dark energy was modeled by means of a phantom fluid with equation of state P=ωρ, with ω<-1. © 2012 American Physical Society.

U2 - 10.1103/PhysRevD.86.083528

DO - 10.1103/PhysRevD.86.083528

M3 - Article

VL - 86

IS - 8

M1 - 083528

ER -