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Parameter study on Kelvin–Helmholtz instability in solar wind type flowing structures

Published online by Cambridge University Press:  01 November 2006

R. Miteva
Affiliation:
Astrophysikalisches Institut Potsdam, an der Sternwarte 16, 14482 Potsdam, Germany email:rmiteva@aip.de Department of Physics, Sofia University, 5 J. Bourchier blvd., 1164 Sofia, Bulgaria
S. Ivanovski
Affiliation:
Astrophysikalisches Institut Potsdam, an der Sternwarte 16, 14482 Potsdam, Germany email:rmiteva@aip.de
I. Zhelyazkov
Affiliation:
Department of Physics, Sofia University, 5 J. Bourchier blvd., 1164 Sofia, Bulgaria
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Abstract

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The stability behaviour of the wave modes that propagate in the solar wind plasma is considered in the framework of the Hall-magnetohydrodynamics. The Hall-MHD theory extends the wave frequency limit up to or higher than the ion cyclotron frequency. Due to the different flow velocities of the adjacent media in the solar wind, a Kelvin–Helmholtz instability is naturally expected to arise. The behaviour of the wave modes due to this particular kind of instability is studied under solar wind conditions typical for 1 AU. This is a preliminary study on the stability problem in the solar wind flowing structures and it could be relevant for the interplanetary and space weather research.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union