  In molecular cloud cores, the cosmic ray (CR) induced sputtering via CR
ion-icy grain collision is one of the desorption processes for ice molecules
from mantles around dust grains. The efficiency of this process depends on the
incident CR ion properties as well as the physicochemical character of the ice
mantle. Our main objective is the examination of the sputtering efficiency for
H$_2$O and CO ices found in molecular cloud cores. In the calculation routine,
we consider a multi-dimensional parameter space that consists of thirty CR ion
types, five different CR ion energy flux distributions, two separate ice mantle
components (pure H$_2$O and CO), three ice formation states, and two sputtering
regimes (linear and quadratic). We find that the sputtering behavior of H$_2$O
and CO ices is dominated by the quadratic regime rather than the linear regime,
especially for CO sputtering. The sputtering rate coefficients for H$_2$O and
CO ices show distinct variations with respect to the adopted CR ion energy flux
as well as the grain size-dependent mantle depth. The maximum radius of the
cylindrical latent region is quite sensitive to the effective electronic
stopping power. The track radii for CO ice are much bigger than H$_2$O ice
values. In contrast to the H$_2$O mantle, even relatively light CR ions ($Z
\geq 4$) may lead to a track formation within the CO mantle, depending on ${\rm
S_{\rm e,eff}}$. We suggest that the latent track formation threshold can be
assumed as a separator between the linear and the quadratic regimes for
sputtering.
