Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-14T05:08:39.426Z Has data issue: false hasContentIssue false
  • English
  • Français

The Kelvin-Helmholtz Instability in Smoothed-Particle Hydrodynamics

Published online by Cambridge University Press:  01 August 2006

Veronika Junk ,
Fabian Heitsch  and
Thorsten Naab
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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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).

Keywords

hydrodynamicsinstabilitiessimulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 210
Copyright
Copyright © International Astronomical Union 2007

References

Murray, S. D., White, S. D. M., Blondin, J. M., & Lin, D. N. C. 1993, ApJ, 407, 588.CrossRefGoogle Scholar
Chandrasekhar, S. 1961, Hydrodynamic and Hydromagnetic Stability, Dover Publication.Google Scholar
Prendergast, K. H., & Xu, K., 1993, J. Comp. Phys., 109, 53.CrossRefGoogle Scholar
Slyz, A. D., & Prendergast, K. H. 1999, A&AS, 139, 199.Google Scholar
Slyz, A. D., Devriendt, J. E. G., Bryan, G., Heitsch, F. & Silk, J. 2006, MNRAS, submitted.Google Scholar
Heitsch, F., Slyz, A. D., Devriendt, J. E. G., Hartmann, L., & Burkert, A. 2006, ApJ, submitted.Google Scholar