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Magnetic fields and Turbulence in Star Formation using Smoothed Particle Hydrodynamics

Published online by Cambridge University Press:  27 April 2011

Daniel J. Price
Daniel J. Price*
Affiliation:
Centre for Stellar and Planetary Astrophysics, Monash University, Clayton Vic 3800, Australia. email: daniel.price@monash.edu
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Abstract

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Firstly, we give a historical overview of attempts to incorporate magnetic fields into the Smoothed Particle Hydrodynamics method by solving the equations of Magnetohydrodynamics (MHD), leading an honest assessment of the current state-of-the-art in terms of the limitations to performing realistic calculations of the star formation process. Secondly, we discuss the results of a recent comparison we have performed on simulations of driven, supersonic turbulence with SPH and Eulerian techniques. Finally we present some new results on the relationship between the density variance and the Mach number in supersonic turbulent flows, finding σ2ln ρ = ln(1 + b22 with b = 0.33 up to Mach 20, consistent with other numerical results at lower Mach number (Lemaster & Stone 2008) but inconsistent with observational constraints on σρ and in Taurus and IC5146.

Keywords

magnetic fieldsmagnetohdyrodynamics (MHD)turbulencemethods: numericalISM: clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 169 - 177
Copyright
Copyright © International Astronomical Union 2011

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