Anisotropic $2$-form dark energy. (arXiv:1902.05846v1 [hep-th])
<a href="http://arxiv.org/find/hep-th/1/au:+Almeida_J/0/1/0/all/0/1">Juan P. Beltrán Almeida</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Guarnizo_A/0/1/0/all/0/1">Alejandro Guarnizo</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Kase_R/0/1/0/all/0/1">Ryotaro Kase</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Tsujikawa_S/0/1/0/all/0/1">Shinji Tsujikawa</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Valenzuela_Toledo_C/0/1/0/all/0/1">César A. Valenzuela-Toledo</a>
We study the dynamics of dark energy in the presence of a 2-form field
coupled to a canonical scalar field $phi$. We consider the coupling
proportional to $e^{-mu phi/M_{rm pl}} H_{alpha beta gamma}H^{alpha
beta gamma}$ and the scalar potential $V(phi) propto e^{-lambda
phi/M_{rm pl}}$, where $H_{alpha beta gamma}$ is the 2-form field
strength, $mu, lambda$ are constants, and $M_{rm pl}$ 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 $lambda geq {cal O}(1)$, it is possible to realize the dark energy
equation of state $w_{rm DE}$ close to $-1$ at low redshifts for $mu gg
lambda$. The existence of anisotropic hair and the oscillating behavior of
$w_{rm DE}$ are key features for distinguishing our scenario from other dark
energy models like quintessence.
We study the dynamics of dark energy in the presence of a 2-form field
coupled to a canonical scalar field $phi$. We consider the coupling
proportional to $e^{-mu phi/M_{rm pl}} H_{alpha beta gamma}H^{alpha
beta gamma}$ and the scalar potential $V(phi) propto e^{-lambda
phi/M_{rm pl}}$, where $H_{alpha beta gamma}$ is the 2-form field
strength, $mu, lambda$ are constants, and $M_{rm pl}$ 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 $lambda geq {cal O}(1)$, it is possible to realize the dark energy
equation of state $w_{rm DE}$ close to $-1$ at low redshifts for $mu gg
lambda$. The existence of anisotropic hair and the oscillating behavior of
$w_{rm DE}$ are key features for distinguishing our scenario from other dark
energy models like quintessence.
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