  Aims: I report results in numerical simulations of star-disk magnetospheric
interaction. A thin accretion disk with corona above a rotating stellar surface
is simulated in a parameter study, to find trends in the angular momentum flux.
The results are presented in the case of Young Stellar Objects, but they can be
rescaled to other objects with similar geometry.
  Methods: In the performed resistive and viscous magneto-hydrodynamic
simulations, a quasi-stationary state is reached in the cases with different
parameters. Angular momentum fluxes in the different components of the flow are
computed, to compare the results.
  Results: Results in the simulations are presented with the matter density
distribution and magnetic field geometry displayed in an `Atlas' of solutions.
The torque exerted on the star is computed, together with the angular momentum
flux loaded into outflow, in the cases when a conical outflow is formed. In the
studied part of the parameter space, I find trends in both components of the
flow.
