# Theoretical model of hydrodynamic jet formation from accretion disks with turbulent viscosity

## TL;DR

This paper presents an analytic theoretical model for hydrodynamic jets from protostellar disks, linking jet properties with disk flow characteristics through self-similar solutions and turbulent viscosity extension.

## Contribution

It introduces a novel analytic framework connecting jet ejection features directly with accretion disk flow properties using Beltrami-Bernoulli configurations.

## Key findings

- Jet ejection velocity depends on turbulence parameter.
- Jet velocity increases as local sound speed decreases.
- Solutions enable analysis of protostellar jet and disk flow relationships.

## Abstract

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.