  The rotational evolution of accreting pre-main-sequence stars is influenced
by its magnetic interaction with its surrounding circumstellar disk. Using the
PLUTO code, we perform 2.5D magnetohydrodynamic, axisymmetric, time-dependent
simulations of star-disk interaction---with an initial dipolar magnetic field
structure, and a viscous and resistive accretion disk---in order to model the
three mechanisms that contribute to the net stellar torque: accretion flow,
stellar wind, and magnetospheric ejections (periodic inflation and reconnection
events). We investigate how changes in the stellar magnetic field strength,
rotation rate, and mass accretion rate (changing the initial disk density)
affect the net stellar torque. All simulations are in a net spin-up regime. We
fit semi-analytic functions for the three stellar torque contributions,
allowing for the prediction of the net stellar torque for our parameter regime,
and the possibility of investigating spin-evolution using 1D stellar evolution
codes. The presence of an accretion disk appears to increase the efficiency of
stellar torques compared to isolated stars, for cases with outflow rates much
smaller than accretion rates, because the star-disk interaction opens more of
the stellar magnetic flux compared to that from isolated stars. In our
parameter regime, a stellar wind with a mass loss rate of $\approx 1 \%$ of the
mass accretion rate is capable of extracting $\lesssim 50 \%$ of the accreting
angular momentum. These simulations suggest that achieving spin-equilibrium in
a representative T Tauri case within our parameter regime, e.g., BP Tau, would
require a wind mass loss rate of $\approx 25\%$ of the mass accretion rate.
