  We assess the modification of angular momentum transport in various
configurations of star-disk accreting systems based on numerical simulations
with different parameters. We quantify the torques exerted on a star by the
various components of the flow in our simulations of a star-disk magnetospheric
interaction. We obtained results using different stellar rotation rates, dipole
magnetic field strengths, and resistivities. We probed a part of the parameter
space with slowly rotating central objects, up to 20% of the Keplerian rotation
rate at the equator. Different components of the flow in star-disk
magnetospheric interaction were considered in the study: a magnetospheric wind
(i.e., the ``stellar wind'') ejected outwards from the stellar vicinity, matter
infalling onto the star through the accretion column, and a magnetospheric
ejection launched from the magnetosphere. We also took account of trends in the
total torque in the system and in each component individually. We find that for
all the stellar magnetic field strengths, B$_\star$, the anchoring radius of
the stellar magnetic field in the disk is extended with increasing disk
resistivity. The torque exerted on the star is independent of the stellar
rotation rate, $\Omega_\star$, in all the cases without magnetospheric
ejections. In cases where such ejections are present, there is a weak
dependence of the anchoring radius on the stellar rotation rate, with both the
total torque in the system and torque on the star from the ejection and infall
from the disk onto the star proportional to $\Omega_\star B^3$. The torque from
a magnetospheric ejection is proportional to $\Omega_\star^4$. Without the
magnetospheric ejection, the spin-up of the star switches to spin-down in cases
involving a larger stellar field and faster stellar rotation. The critical
value for this switch is about 10% of the Keplerian rotation rate.
