Dense Regions in Supersonic Isothermal Turbulence

TL;DR

This paper introduces a simple analytical model for dense regions in supersonic isothermal turbulence, supported by simulations, offering new insights into the structure of star-forming clouds.

Contribution

The work presents a novel hydrostatic balance model for dense shock regions in turbulence, validated by simulations, enhancing understanding of astrophysical turbulence structures.

Findings

Model agrees with simulation data

Provides a new conceptual framework

Enhances understanding of star-forming cloud structures

Abstract

The properties of supersonic isothermal turbulence influence a variety of astrophysical phenomena, including the structure and evolution of star forming clouds. This work presents a simple model for the structure of dense regions in turbulence in which the density distribution behind isothermal shocks originates from rough hydrostatic balance between the pressure gradient behind the shock and its deceleration from ram pressure applied by the background fluid. Using simulations of supersonic isothermal turbulence and idealized waves moving through a background medium, we show that the structural properties of dense, shocked regions broadly agree with our analytical model. Our work provides a new conceptual picture for describing the dense regions, which complements theoretical efforts to understand the bulk statistical properties of turbulence and attempts to model the more complex features of star forming clouds like magnetic fields, self-gravity, or radiative properties.