Turbulent entrainment origin of protostellar outflows

TL;DR

This paper presents a theoretical model where turbulent entrainment of ambient gas by stellar winds explains the shape, mass, and velocity of protostellar outflows, emphasizing turbulence's universal role.

Contribution

It introduces a novel turbulent entrainment model for protostellar outflows, incorporating ambient turbulence effects absent in previous models.

Findings

Outflows have conical shapes consistent with the model.

Outflow velocity exceeds ambient gas velocity dispersion.

Outflow opening angle depends on wind strength and turbulence.

Abstract

Protostellar outflow is a prominent process that accompanies the formation of stars. It is generally agreed that wide-angled protostellar outflows come from the interaction between the wind from a forming star and the ambient gas. However, it is still unclear how the interaction takes place. In this work, we theoretically investigate the possibility that the outflow results from interaction between the wind and the ambient gas in the form of turbulent entrainment. In contrast to the previous models, turbulent motion of the ambient gas around the protostar is taken into account. In our model, the ram-pressure of the wind balances the turbulent ram-pressure of the ambient gas, and the outflow consists of the ambient gas entrained by the wind. The calculated outflow from our modelling exhibits a conical shape. The total mass of the outflow is determined by the turbulent velocity of the envelope as well as the outflow age, and the velocity of the outflow is several times higher than the velocity dispersion of the ambient gas. The outflow opening angle increases with the strength of the wind and decreases with the increasing ambient gas turbulence. The outflow exhibits a broad line width at every position. We propose that the turbulent entrainment process, which happens ubiquitously in nature, plays a universal role in shaping protostellar outflows.