Abstract
In this work we derive a general expression for the greybody factor of non-minimally coupled scalar fields in Reissner–Nordström–de Sitter spacetime in low frequency approximation. Greybody factor as a characteristic of effective potential barrier, will be presented. We discuss the role of cosmological constant both, in the absence as well as in the presence of non-minimal coupling. Considering non-minimal coupling as a mass term, its effect on the greybody factor will be discussed. We also elaborate the significance of the results by giving formulae of differential energy rate and general absorption cross section. The greybody factor gives insight into the spectrum of Hawking radiations.
Highlights
The study of asymptotically non-flat spacetime geometries received a lot of attention after it was discovered that our Universe has entered into a new phase of accelerated expansion [1]
Among these non-flat geometries de Sitter spacetime is of great interest due to its rich symmetries and because it could incorporate the accelerated expansion of the Universe due to the presence of non-zero cosmological constant in the Einstein field equations
Due to the structure of de Sitter spacetime inertial observers are surrounded by cosmological horizons, which are a characteristic of spacetimes having positive cosmological constant
Summary
The study of asymptotically non-flat spacetime geometries received a lot of attention after it was discovered that our Universe has entered into a new phase of accelerated expansion [1] Among these non-flat geometries de Sitter spacetime is of great interest due to its rich symmetries and because it could incorporate the accelerated expansion of the Universe due to the presence of non-zero cosmological constant in the Einstein field equations. In this paper we use the simple matching technique to solve the radial equation resulting from the Klein Gordon equation in the background of the Riessner–Nordström–de Sitter black hole In this method we divide the space into two regimes, namely near the black hole horizon and near the cosmological horizon and find solutions for radial equations in both the regimes separately. 3 we compute the greybody factor, starting from near black hole horizon solution, near cosmological horizon solution, and matching them at an intermediate point.
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