  We linearly perturb advective isothermal transonic accretion onto rotating
astrophysical black holes to study the emergence of the relativistic acoustic
spacetime and to investigate how the salient features of such spacetime get
influenced by the spin angular momentum of the black hole. We have perturbed
three different quantities - the velocity potential, the mass accretion rate
and the relativistic Bernoulli's constant to show that the acoustic metric
obtained for these three cases are same up to a conformal factor. By
constructing the required causal structures, it has been demonstrated that the
acoustic black holes are formed at the transonic points of the flow and
acoustic white holes are formed at the shock location. The corresponding
acoustic surface gravity has been computed in terms of the relevant accretion
variables and the background metric elements. The linear stability analysis of
the background stationary flow has been performed.
