Greybody factors for a minimally coupled massless scalar field in Einstein-Born-Infeld dilaton spacetime

Abstract

We have analyzed in detail the propagation of a minimally coupled massless scalar field in the gravitational background of a four-dimensional Einstein-Born-Infeld dilaton charged black hole. We have obtained analytical expressions for the absorption cross section as well as for the decay rate for the scalar field in the aforementioned spacetime, and we have shown graphically its behavior for different values of the free parameters of the theory.

Scale-dependent ( $$2+1$$ 2 + 1 )-dimensional electrically charged black holes in Einstein-power-Maxwell theory

“…In three dimensions the generic black hole solution without imposing the traceless condition has been found in [21], while black hole solutions in linear Einstein-Maxwell theory are given in [29,30]. Other interesting solutions and properties of black holes in the presence of power-Maxwell theory have been found in [22,25,[31][32][33][34], whereas some topological black hole solutions with powerlaw Maxwell fields have been investigated in [35][36][37], as well as Born-Infeld theory in [38,39]. Interesting features arise from a study of the thermodynamic properties of EpM black holes, as discussed in [32].…”

Greybody factors for a spherically symmetric Einstein-Gauss-Bonnet–de Sitter black hole

“…The comparison of the analytical result with the numerical result was done in [35]. For more studies, see [36][37][38][39][40][41][42][43][44][45][46][47][48]. Adopting a similar radial coordinate, we are able to derive the analytical results for the greybody factors for arbitrary partial modes of a scalar field in the EGB-dS black hole spacetime as well.…”

Black hole shadow of a rotating polytropic black hole by the Newman–Janis algorithm without complexification

“…In particular, α r corresponds to the most right value of α and the pair (α t , β t ) stands for coordinates of the top of the shadow [60]. With all the quantities defined in this section, the emission rate [56,[61][62][63][64][65][66][67] can be calculated by…”