To appear in the Astropysical Journal
We investigate, by means of three dimensional compressible magnetohydrodynamic numerical simulations, the interaction of Kelvin-Helmholtz (KH) and current-driven (CD) instabilities in a magnetized cylindrical jet configuration. The jet has a supersonic axial flow, sheared in the radial direction, and is embedded in an helical magnetic field. The strength of the axial magnetic field component is chosen to be weak, in accord with the `weak field regime' previously defined by Ryu, Jones & Frank for uniformly magnetized configurations. We follow the time evolution of a periodic section where the jet surface is perturbed at m = +/- 1 azimuthal mode numbers. An m = -1 KH surface mode linearly develops dominating the m = +1 KH one, in agreement with results obtained using an independent ideal stability code. This lifted degeneracy, due to the presence of the helical field, leads nonlinearly to clear morphological differences in the jet deformation as compared to uniformly magnetized configurations. As predicted by stability results, an m = -1 CD instability also develops linearly inside the jet core for configurations having a small enough magnetic pitch length. As time proceeds, this magnetic mode interacts with the KH vortical structures and significantly affects the further nonlinear evolution. The magnetic field deformation induced by the CD instability provides a stabilizing effect through its azimuthal component B_theta. This helps to saturate the KH vortices in the vicinity of the jet surface. Beyond saturation, the subsequent disruptive effect on the flow is weaker than in cases having similar uniform and helical magnetic field configurations without CD mode. We discuss the implications of this stabilizing mechanism for the stability of astrophysical jets.