Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-24T15:55:36.842Z Has data issue: false hasContentIssue false
  • English
  • Français

Kelvin-Helmholtz instability in MHD flows

Published online by Cambridge University Press:  01 November 2006

A. H. Khater ,
D. K. Callebaut  and
A. R. Seadawy
A. H. Khater
Affiliation:
Department of Mathematics, Faculty of Science, Beni-Suef University, Beni-Suef, Egypt Department Natuurkunde, CGB, University of Antwerp, B-2020 Antwerp, Belgium
D. K. Callebaut
Affiliation:
Department Natuurkunde, CGB, University of Antwerp, B-2020 Antwerp, Belgium
A. R. Seadawy
Affiliation:
Department of Mathematics, Faculty of Science, Beni-Suef University, Beni-Suef, Egypt
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.

The Kelvin-Helmholtz instability (KHI) could be a potential source for some of the Alfvénic fluctuations observed in the solar wind. The nonlinear evolution of KHI is examined in 2+1 dimensions in the context of magnetohydrodynamics. We derived a nonlinear Schródinger equation (NLSE) and we obtained soliton solutions of this 2+1 dimensions NLSE.

Keywords

MHDKelvin-Helmholtz instabilitysolar windplanetary interiors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 313 - 315
Copyright
© 2006 International Astronomical Union