Evolution of axial perturbations in a non-rotating uncharged primordial black hole

We derive the equation governing the axial-perturbations in the space-time of a non-rotating uncharged primordial black hole (PBH), produced in early Universe, whose metric has been taken as the generalized McVittie metric. The generalized McVittie metric is a cosmological black hole metric, proposed by Faraoni and Jacques in 2007 (Phys. Rev. D 76:063510, 2007). This describes the space-time of a Schwarzschild black hole embedded in FLRW-Universe, while allowing its mass-change. Our derivation has basic similarities with the procedure of derivation of Chandrasekhar, for deriving the Regge-Wheeler equation for Schwarzschild metric (Chandrasekhar The Mathematical Theory of Black holes, Oxford University Press, New York, 1983); but it has some distinct differences with that due to the complexity and time-dependency of the generalized McVittie metric. We show that after applying some approximations which are very well valid in the early radiation-dominated Universe, the overall equation governing the axial perturbations can be separated into radial and angular parts, among which the radial part is the intended one, as the angular part is identical to the case of Schwarzschild metric as expected. We identify the potential from the Schrödinger-like format of the equation and draw some physical interpretation from it.