Non-Abelian S-term dark energy and inflation
We study the role that a cosmic triad in the generalized SU(2) Proca theory, specifically in one of the pieces of the Lagrangian that involves the symmetric version Sμν of the gauge field strength tensor Fμν, has on dark energy and primordial inflation. Regarding dark energy, the triad behaves asy...
| Autor Principal: | Rodríguez, Yeinzon |
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| Otros Autores: | Navarro, Andrés A. |
| Formato: | Generación de Nuevo Conocimiento: Artículos publicados en revistas especializadas - Electrónicos |
| Publicado: |
2019
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| Materias: | |
| Acceso en línea: |
Rodríguez, Y., & Navarro, A. A. (2018). Non-abelian S-term dark energy and inflation doi:10.1016/j.dark.2018.01.003 |
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| Sumario: |
We study the role that a cosmic triad in the generalized SU(2) Proca theory, specifically in one of the
pieces of the Lagrangian that involves the symmetric version Sμν of the gauge field strength tensor Fμν,
has on dark energy and primordial inflation. Regarding dark energy, the triad behaves asymptotically
as a couple of radiation perfect fluids whose energy densities are negative for the S term but positive
for the Yang–Mills term. This leads to an interesting dynamical fine-tuning mechanism that gives rise
to a combined equation of state parameter ω ≃ −1 and, therefore, to an eternal period of accelerated
isotropic expansion for an ample spectrum of initial conditions. Regarding primordial inflation, one of the
critical points of the associated dynamical system can describe a prolonged period of isotropic slow-roll
inflation sustained by the S term. This period ends up when the Yang–Mills term dominates the energy
density leading to the radiation dominated epoch. Unfortunately, in contrast to the dark energy case, the
primordial inflation scenario is strongly sensitive to the coupling constants and initial conditions. The
whole model, including the other pieces of the Lagrangian that involve Sμν, might evade the recent strong
constraints coming from the gravitational wave signal GW170817 and its electromagnetic counterpart
GRB 170817A. |
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