TY - JOUR
T1 - Anisotropic 2-form dark energy
AU - Beltrán Almeida, Juan P.
AU - Guarnizo, Alejandro
AU - Kase, Ryotaro
AU - Tsujikawa, Shinji
AU - Valenzuela-Toledo, César A.
N1 - Funding Information:
This work was partly supported by COLCIENCIAS grant 110671250405 RC FP44842-103-2016 and by COLCIENCIAS grant 110278258747 RC-774-2017 (DAAD-Procol program). JPBA acknowledges support from Universidad Antonio Nariño grant 2017239 and thanks Tokyo University of Science for kind hospitality at early stages of this project. RK is supported by the Grant-in-Aid for Young Scientists B of the JSPS No. 17K14297 . ST is supported by the Grant-in-Aid for Scientific Research Fund of the JSPS No. 16K05359 and MEXT KAKENHI Grant-in-Aid for Scientific Research on Innovative Areas “Cosmic Acceleration” (No. 15H05890 ).
Publisher Copyright:
© 2019 The Author(s)
PY - 2019/6/10
Y1 - 2019/6/10
N2 - We study the dynamics of dark energy in the presence of a 2-form field coupled to a canonical scalar field ϕ. We consider the coupling proportional to e −μϕ/M pl H αβγ H αβγ and the scalar potential V(ϕ)∝e −λϕ/M pl , where H αβγ is the 2-form field strength, μ,λ are constants, and M pl is the reduced Planck mass. We show the existence of an anisotropic matter-dominated scaling solution followed by a stable accelerated fixed point with a non-vanishing shear. Even if λ≥O(1), it is possible to realize the dark energy equation of state w DE close to −1 at low redshifts for μ≫λ. The existence of anisotropic hair and the oscillating behavior of w DE are key features for distinguishing our scenario from other dark energy models like quintessence.
AB - We study the dynamics of dark energy in the presence of a 2-form field coupled to a canonical scalar field ϕ. We consider the coupling proportional to e −μϕ/M pl H αβγ H αβγ and the scalar potential V(ϕ)∝e −λϕ/M pl , where H αβγ is the 2-form field strength, μ,λ are constants, and M pl is the reduced Planck mass. We show the existence of an anisotropic matter-dominated scaling solution followed by a stable accelerated fixed point with a non-vanishing shear. Even if λ≥O(1), it is possible to realize the dark energy equation of state w DE close to −1 at low redshifts for μ≫λ. The existence of anisotropic hair and the oscillating behavior of w DE are key features for distinguishing our scenario from other dark energy models like quintessence.
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U2 - 10.1016/j.physletb.2019.05.008
DO - 10.1016/j.physletb.2019.05.008
M3 - Article
AN - SCOPUS:85065507571
SN - 0370-2693
VL - 793
SP - 396
EP - 404
JO - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
JF - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
ER -