FRONTIERS IN COMPUTATIONAL ASTROPHYSICS

Particle and Flames in Radiative and Magnetic Flows

October 11-15, 2010
Lyon, France

Contribution of C. Federrath

Title

Modeling interstellar turbulence and star formation

Topics

"Stellar structure and evolution"

Keywords

Turbulence

Abstract

It is often believed that the particular way of turbulence forcing does not make a difference in terms of statistical properties of the turbulent flow. I will present hydrodynamical simulations of supersonic turbulence in which the turbulence was driven with either solenoidal (divergence-free) and or compressive (curl-free) forcing. The obtained density distribution has a three times larger standard deviation for compressive forcing, even at the same RMS Mach number. In a set of self-gravitating turbulence simulations, including sink particles to model the collapse and accretion of dense gas, I show that the star formation rate is more than an order of magnitude larger for compressive forcing than for solenoidal forcing. Real clouds show turbulence statistics in between those two limiting cases, but purely solenoidal forcing seems clearly inconsistent with the observations.

Talk