  In our previous work (Paper I) we applied several models of high-frequency
quasi-periodic oscillations (HF QPOs) to estimate the spin of the central
compact object in three Galactic microquasars assuming the possibility that the
central compact body is a super-spinning object (or a naked singularity) with
external spacetime described by Kerr geometry with a dimensionless spin
parameter $a\equiv cJ/GM^2>1$. Here we extend our consideration, and in a
consistent way investigate implications of a set of ten resonance models so far
discussed only in the context of $a<1$. The same physical arguments as in Paper
I are applied to these models, i.e. only a small deviation of the spin estimate
from $a=1$, $a\gtrsim 1$, is assumed for a favoured model. For five of these
models that involve Keplerian and radial epicyclic oscillations we find the
existence of a unique specific QPO excitation radius. Consequently, there is a
simple behaviour of dimensionless frequency $M\times\nu_{U}(a)$ represented by
a single continuous function having solely one maximum close to $a\gtrsim1$.
Only one of these models is compatible with the expectation of $a\gtrsim 1$.
The other five models that involve the radial and vertical epicyclic
oscillations imply the existence of multiple resonant radii. This signifies a
more complicated behaviour of $M\times\nu_{U}(a)$ that cannot be represented by
single functions. Each of these five models is compatible with the expectation
of $a\gtrsim 1$.
