Magnetic fields and turbulence in star formation using smoothed particle hydrodynamics

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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 I?2ln = 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 I?p and in Taurus and IC5146.
Original languageEnglish
Title of host publicationProceedings of the International Astronomical Union [P]
EditorsJoao Alves, Bruce G Elmegreen, Josep M Girart, Virginia Trimble
Place of PublicationUnited Kingdom
PublisherCambridge University Press
Pages169 - 178
Number of pages10
ISBN (Print)1743-9213
Publication statusPublished - 2011
EventInternational Astronomical Union Symposium 2010 - Barcelona Catalonia, Spain
Duration: 31 May 20104 Jun 2010


ConferenceInternational Astronomical Union Symposium 2010
Abbreviated titleIAU Symposium 2010
CityBarcelona Catalonia

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