  We develop the theoretical model for the analytic description of hydrodynamic
jets from protostellar disks employing the Beltrami-Bernoulli flow
configuration of disk-jet structure. For this purpose we extend the standard
turbulent viscosity prescription and derive several classes of analytic
solutions using the flow parametrization in self-similar variables. Derived
solutions describe the disk-jet structure, where for the first time jet
properties are analytically linked with the properties of the accretion disk
flow. The ratio of the jet ejection and disk accretion velocities is controlled
by the turbulence parameter, while the ejection velocity increases with the
decrease of local sound velocity and the jet launching radius. Derived
solutions can be used to analyze the astrophysical jets from protostellar
accretion disks and link the properties of outflows with the local
observational properties of accretion disk flows.
