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The Kelvin-Helmholtz Instability in Smoothed-Particle Hydrodynamics

Published online by Cambridge University Press:  01 August 2006

Veronika Junk
Affiliation:
University Observatory Munich, Scheinerstrasse 1, 81679 Munich, Germany email: vjunk@usm.uni-muenchen.de
Fabian Heitsch
Affiliation:
University Observatory Munich, Scheinerstrasse 1, 81679 Munich, Germany email: vjunk@usm.uni-muenchen.de Department of Astronomy, University of Michigan, 500 Church St, Ann Arbor, MI 48109-1042, USA
Thorsten Naab
Affiliation:
University Observatory Munich, Scheinerstrasse 1, 81679 Munich, Germany email: vjunk@usm.uni-muenchen.de
Corresponding
E-mail address:
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Abstract

Smoothed Particle Hydrodynamics (SPH) simulations are a powerful tool to investigate hydrodynamical processes in astrophysics such as the formation of galactic disks. Dense gas clouds raining on the forming disk are possibly disrupted by Kelvin-Helmholtz-Instabilities (KHI). To understand the evolution of the halo clouds, we have to ascertain the capability of SPH to treat the KHI correctly, since SPH-methods tend to suffer from an innate surface tension and viscosity effects, both of which could dampen the KHI. We analytically derive a growth rate of the KHI including surface tension and viscosity in the linear regime, and compare this growth rate to results of numerical simulations by an SPH method and a grid-based method. We find that SPH in some cases suppresses the KHI (Junk et al., in prep).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

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Heitsch, F., Slyz, A. D., Devriendt, J. E. G., Hartmann, L., & Burkert, A. 2006, ApJ, submitted.Google Scholar
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