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Article Contents

ABSTRACT

1.INTRODUCTION

2.DIAGNOSTICS OF TURBULENCE IN THE DENSE INTERSTELLAR MEDIUM

3.POWER SOURCES FOR INTERSTELLAR TURBULENCE

4.THEORY OF INTERSTELLAR TURBULENCE
4.1.What is Turbulence and Why Is It So Complicated?
4.2.Basic Equations
4.3.Statistical Closure Theories
4.4.Solenoidal and Compressible Modes
4.5.Global Inviscid Quadratic Invariants are Fundamental Constraints on the Nature of Turbulent Flows
4.6.Scale-invariant Kinetic Energy Flux and Scaling Arguments for the Power Spectrum
4.7.Intermittency and Structure Function Scaling
4.8.Details of the Energy Cascade: Isotropy and Independence of Large and Small Scales
4.9.Velocity Probability Distribution
4.10.Turbulent "Pressure"
4.11.Below the Collision Mean Free Path
4.12.MHD Turbulence Theory: Power Spectra
4.13.The Anisotropic Kolmogorov Model

5.SIMULATIONS OF INTERSTELLAR TURBULENCE
5.1.Introduction
5.2.Scaling Relations
5.3.Decay of Supersonic MHD Turbulence
5.4.The Density Probability Distribution
5.5.Energy Cascades
5.6.Compressible versus Solenoidal Motions
5.7.Filamentary Structure
5.8.Thermal Instability and Thermal Phases
5.9.Supernova-Driven Turbulence
5.10.The Role of Self-Gravity in the ISM
5.11.Formation of Star Clusters and the IMF
5.12.Rotation and Binary Star Formation
5.13.Effects of Magnetic Fields on Interstellar Turbulence
5.14.Turbulent Rotating Galaxy Disk Simulations

6.SUMMARY AND REFLECTIONS

REFERENCES