David A. Tilley

The formation of star clusters – I. Three-dimensional simulations of hydrodynamic turbulence

We present the results of a series of numerical simulations of compressible, self-gravitating hydrodynamic turbulence of cluster-forming clumps in molecular clouds. We examine the role that turbulence has in the formation of gravitationally bound cores, studying the dynamical state, internal structure and bulk properties of these cores. Complex structure in turbulent clumps is formed provided that the damping time of the turbulence,

The Formation of Star Clusters I: 3D Simulations of Hydrodynamic Turbulence

t_{damp}

The formation of star clusters – II. 3D simulations of magnetohydrodynamic turbulence in molecular clouds

is longer than the gravitational free-fall time

Gravitational Collapse of Filamentary Magnetized Molecular Clouds

t_{ff}

Dust settling in magnetorotationally driven turbulent discs – I. Numerical methods and evidence for a vigorous streaming instability

in a region. We find a variety of density and infall velocity structures among the cores in the simulation, including cores that resemble the Larson-Penston collapse of an isothermal sphere (

Dust stratification in young circumstellar disks

\rho \propto r^{-2}

Direct evidence for two-fluid effects in molecular clouds

) as well as cores that resemble the McLaughlin-Pudritz collapse of logatropic spheres (

A two-fluid method for ambipolar diffusion

\rho \propto r^{-1}

Simulating anisotropic thermal conduction in supernova remnants - II. Implications for the interstellar medium

). The specific angular momentum profiles range between

Simulations of mixed-morphology supernova remnants with anisotropic thermal conduction

j \propto r^{1} - r^{2}