In this study, we investigated the effects of incorporating barotropic fluids
on cosmological solutions within the general relativity (GR) framework. Noi
proposed a modified version of the barotropic fluid with the EoS, $p=\zeta _0
\rho +\zeta _1 \rho \left(t-t_0\right){}^{-2 n}$, where $\zeta_0$, $\zeta_1$,
$t_0$ and $n$ are some constants. Our goal is to explore if this type of EoS
might help explain the universe’s development, concentrating on the scenario
where the universe bounces instead of singularities. Interestingly the generic
solutions derived from our model are sufficiently adaptable to illustrate the
bounce scenario, cosmic inflation and late-time dark-energy behaviour. The
parameters $\zeta_0$, $\zeta_1$, $t_0$, and $n$ define the universe’s phase in
this non-singular solution. We investigated several elements of cosmic
development, including as the energy density, deceleration parameter, E
energy conditions, in order to validate our model. Stability analysis showed
that the perturbations approach to zero as the time evolves, indicating the
model is stable under scalar perturbation. Inoltre, we looked at the
statefinder diagnostics and Hubble flow dynamics to get more understanding of
the model’s dark energy and inflationary behaviour, rispettivamente. Inoltre,
we conducted a study of the models’ relevance to the observational datasets
from BAO, DESI and Pantheon+SH0ES.

Questo articolo esplora i giri e le loro implicazioni.

Scarica PDF: