$alpha$ attractors in Quintessential Inflation motivated by Supergravity. (arXiv:2103.07892v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Salo_L/0/1/0/all/0/1">Llibert Aresté Saló</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benisty_D/0/1/0/all/0/1">David Benisty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guendelman_E/0/1/0/all/0/1">Eduardo I. Guendelman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haro_J/0/1/0/all/0/1">Jaume de Haro</a>
An exponential kind of quintessential inflation potential motivated by
supergravity is studied. This type belongs to the class of {alpha}-attractor
models. The model was studied for the first time by Dimopoulos and Owen in [J.
Cosmol. Astropart. Phys. 06 (2017) 027], in which the authors introduced a
negative cosmological constant in order to ensure a zero-vacuum energy density
at late times. However, in this paper, we disregard this cosmological constant,
showing that the obtained results are very close to the ones obtained recently
in the context of Lorentzian quintessential inflation and thus depicting with
great accuracy the early- and late-time acceleration of our Universe. The model
is compatible with the recent observations. Finally, we review the treatment of
the {alpha}-attractor and we show that our potential depicts the late time
cosmic acceleration with an effective equation of state equal to -1.
An exponential kind of quintessential inflation potential motivated by
supergravity is studied. This type belongs to the class of {alpha}-attractor
models. The model was studied for the first time by Dimopoulos and Owen in [J.
Cosmol. Astropart. Phys. 06 (2017) 027], in which the authors introduced a
negative cosmological constant in order to ensure a zero-vacuum energy density
at late times. However, in this paper, we disregard this cosmological constant,
showing that the obtained results are very close to the ones obtained recently
in the context of Lorentzian quintessential inflation and thus depicting with
great accuracy the early- and late-time acceleration of our Universe. The model
is compatible with the recent observations. Finally, we review the treatment of
the {alpha}-attractor and we show that our potential depicts the late time
cosmic acceleration with an effective equation of state equal to -1.
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