  We present steady-state calculations of self-similar magnetized accretion
discs driving cold, adiabatic, non-relativistic jets. For the first time, both
the magnetic torque due to the jets and a turbulent "viscous" torque are taken
into account. This latter torque allows a dissipation of the accretion power as
radiation at the disc surfaces, while the former predominantly provides jets
with power.
  The parameter space of these structures has been explored. It is
characterized by four free parameters, namely the disc aspect ratio and three
MHD turbulence parameters, related to the anomalous magnetic diffusivities and
viscosity. It turns out that launching cold jets from thin, dissipative discs
implies anisotropic turbulent dissipation. Jets that asymptotically reach a
high Alfvenic Mach number are only produced by weakly dissipative discs.
  We obtained general analytical relations between disc and jet quantities that
must be fulfilled by any steady-state model of cold jets, launched from a large
radial extension of thin discs. We also show that such discs cannot have a
dominant viscous torque. This is because of the chosen geometry, imposing the
locus of the Alfven surface.
  Some observational consequences of these cold magnetized accretion-ejection
structures are also briefly discussed.
