  In the present paper, we have investigated the motion of charged particles
together with magnetic dipoles to determine how well the spacetime deviation
parameter $\epsilon$ and external uniform magnetic field can mimic the spin of
a rotating Kerr black hole. Investigation of charged particle motion has shown
that the deviation parameter $\epsilon$ in the absence of external magnetic
fields can mimic the rotation parameter of Kerr spacetime up to $a/M
\approx0.5$. The combination of external magnetic field and deviation parameter
can do even a better job mimicking the rotation parameter up to
$a/M\simeq0.93$, which corresponds to the rapidly rotating case. Study of the
dynamics of magnetic dipoles around quasi-Schwarzschild black holes in the
external magnetic field has shown that there are degeneracy values of ISCO
radius of test particles at $\epsilon_{cr}>\epsilon\geq 0.35$ which may lead to
two different values of the innermost stable circular orbit (ISCO) radius. When
the deviation parameter is in the range of $\epsilon \in (-1,\ 1)$, it can
mimic the spin of a rotating Kerr black hole in the range $a/M \in (0.0537, \
0.3952)$ for magnetic dipoles with values of magnetic coupling parameter $\beta
\in [-0.25,\ 0.25]$ in corotating orbits.
