Kaniadakis holographic dark energy and cosmology. (arXiv:2109.09181v2 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Drepanou_N/0/1/0/all/0/1">Niki Drepanou</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Lymperis_A/0/1/0/all/0/1">Andreas Lymperis</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Saridakis_E/0/1/0/all/0/1">Emmanuel N. Saridakis</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Yesmakhanova_K/0/1/0/all/0/1">Kuralay Yesmakhanova</a>
We construct a holographic dark energy scenario based on Kaniadakis entropy,
which is a generalization of Boltzmann-Gibbs entropy that arises from
relativistic statistical theory and is characterized by a single parameter $K$
which quantifies the deviations from standard expressions, and we use the
future event horizon as the Infrared cutoff. We extract the differential
equation that determines the evolution of the effective dark energy density
parameter, and we provide analytical expressions for the corresponding
equation-of-state and deceleration parameters. We show that the universe
exhibits the standard thermal history, with the sequence of matter and
dark-energy eras, while the transition to acceleration takes place at
$zapprox0.6$. Concerning the dark-energy equation-of-state parameter we show
that it can have a rich behavior, being quintessence-like, phantom-like, or
experience the phantom-divide crossing in the past or in the future. Finally,
in the far future dark energy dominates completely, and the asymptotic value of
its equation of state depends on the values of the two model parameters.
We construct a holographic dark energy scenario based on Kaniadakis entropy,
which is a generalization of Boltzmann-Gibbs entropy that arises from
relativistic statistical theory and is characterized by a single parameter $K$
which quantifies the deviations from standard expressions, and we use the
future event horizon as the Infrared cutoff. We extract the differential
equation that determines the evolution of the effective dark energy density
parameter, and we provide analytical expressions for the corresponding
equation-of-state and deceleration parameters. We show that the universe
exhibits the standard thermal history, with the sequence of matter and
dark-energy eras, while the transition to acceleration takes place at
$zapprox0.6$. Concerning the dark-energy equation-of-state parameter we show
that it can have a rich behavior, being quintessence-like, phantom-like, or
experience the phantom-divide crossing in the past or in the future. Finally,
in the far future dark energy dominates completely, and the asymptotic value of
its equation of state depends on the values of the two model parameters.
http://arxiv.org/icons/sfx.gif
