  We use Monte Carlo $\Lambda$CDM assembly histories, minor-merger N-body
simulations and empirical relations between halo mass and the globular cluster
(GC) abundance to study the kinematical properties of halo GCs in massive
galaxies, with $M_{vir}(z=0)=10^{13.5}M_\odot$. While the accreted stellar halo
is dominated by the contributions of massive satellites, we show that
satellites with low virial mass (i.e. low satellite-to-host virial mass ratio,
VMRs) are important contributors to the population of accreted GCs. The
relative contribution of accretion events with low VMRs is highest for the halo
population of blue GCs and gradually decreases for red GCs and accreted stars.
As a consequence of the reduced efficiency of dynamical friction on minor
mergers, our populations of cosmologically accreted blue GCs are systematically
more spatially extended and have higher velocity dispersions than for red GCs,
in agreement with observations. For the same reason, assembly histories
including a higher fraction of minor mergers result in more spatially extended
GC populations. GC line-of-sight velocity distributions featuring negative
values of the kurtosis $\kappa$, as recently observed, are ubiquitous in our
models. Therefore, $\kappa<0$ is not at odds with an accretion scenario, and in
fact a fingerprint of the important contribution of minor mergers. However, our
populations of accreted GCs remain mostly radially biased, with profiles of the
anisotropy parameter $\beta$ that are mildly radial in the center
($\beta(r<10~{\rm kpc})\sim0.2$) and strongly radially anisotropic at large
galactocentric distances ($\beta(r>30~{\rm kpc})\gtrsim0.6$), for both red and
blue populations.
