Shock interactions, turbulence, and the origin of the stellar mass spectrum

TL;DR

This paper reviews how supersonic shock interactions and turbulence shape molecular cloud structures and influence the stellar initial mass function, proposing a simpler shock-based model over traditional turbulence theories.

Contribution

It introduces a physical model emphasizing shock wave interactions as the primary mechanism for cloud structure formation and the origin of the stellar mass spectrum.

Findings

Shock interactions produce dense filaments and vortex sheets.

Log-normal density distribution arises from multiple shock waves.

Vorticity is generated by curved and intersecting shocks.

Abstract

Supersonic turbulence is an essential element in understanding how structure within interstellar gas is created and shaped. In the context of star formation, many computational studies show that the mass spectrum of density and velocity fluctuations within dense clouds, as well as the distribution of their angular momenta, trace their origin to the statistical and physical properties of gas that is lashed with shock waves. In this article, we review the observations, simulations, and theories of how turbulent-like processes can account for structures we see in molecular clouds. We then compare traditional ideas of supersonic turbulence with a simpler physical model involving the effects of multiple shock waves and their interaction in the interstellar medium. Planar intersecting shock waves produce dense filaments, and generate vortex sheets that are essential to create the broad range of density and velocity structure in clouds. As an example, the lower mass behaviour of the stellar initial mass function can be traced to the tendency of a collection of shock waves to build-up a log-normal density distribution (or column density). Vorticity - which is essential to produce velocity structure over a very broad range of length scales in shocked clouds - can also be generated by the passage of curved shocks or intersecting planar shocks through such media. Two major additional physical forces affect the structure of star forming gas - gravity and feedback processes from young stars. Both of these can produce power-law tails at the high mass end of the IMF.