Abstract
In this paper, Quasinormal modes of gravitational perturbation are investigated for the regular Bardeen black hole surrounded by quintessence. Considering the metric of the Bardeen spacetime surrounded by quintessence, we derived the perturbation equation for gravitational perturbation using Regge-Wheeler gauge. The third order Wentzel-Kramers-Brillouin (WKB) approximation method is used to evaluate quasinormal frequencies. Explicitly, the behaviors of the black hole potential and quasinormal modes were plotted. The results show that, due to the presence of quintessence, the gravitational perturbation around the black hole damps more slowly and oscillates more slowly.
Highlights
We can see that our universe is dominated by a mysterious form of energy called “Dark Energy”
It is certainly clear that cosmic inflation requires a period of cosmic acceleration that cannot be described by a cosmological constant [24,25]
Cosmic inflation is understood to be driven by some matter field typically called the “inflaton”, which exhibits an equation of state p = ρq ωq, where p is the pressure, ρq is the density of energy and ωq is the state parameter
Summary
We can see that our universe is dominated by a mysterious form of energy called “Dark Energy”. Cosmic inflation is understood to be driven by some matter field typically called the “inflaton”, which exhibits an equation of state p = ρq ωq , where p is the pressure, ρq is the density of energy and ωq is the state parameter. In this category, we can find quintessence [26,27], phantom [28], k-essence [29], and quintom [30,31] models. Quasinormal modes of gravitational perturbation are investigated for the regular Bardeen black hole surrounded by quintessence.
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