Hostname: page-component-7bb8b95d7b-s9k8s Total loading time: 0 Render date: 2024-09-25T14:50:10.144Z Has data issue: false hasContentIssue false
  • English
  • Français

Propagation of solitary waves and shock wavelength in the pair plasma

Published online by Cambridge University Press:  22 February 2012

BEHROOZ MALEKOLKALAMI  and
TAIMUR MOHAMMADI
BEHROOZ MALEKOLKALAMI
Affiliation:
Department of Physics, University of Kurdistan, P.O. Box 66177-15175, Sanandaj, Iran (b.malakolkalami@uok.ac.ir)
TAIMUR MOHAMMADI
Affiliation:
Department of Physics, University of Kurdistan, P.O. Box 66177-15175, Sanandaj, Iran (b.malakolkalami@uok.ac.ir)
Get access Rights & Permissions [Opens in a new window]

Abstract

The propagation of electrostatic waves is studied in plasma system consisting of pair-ions and stationary additional ions in presence of the Sagdeev potential (pseudopotential) as function of electrostatic potential (pseudoparticle). It is remarked that both compressive and rarefective solitary waves can be propagated in this plasma system. These electrostatic solitary waves, however, cannot be propagated if the density of stationary ions increases from one critical value or decreases from another when the temperature and the Mach number are fixed. Also, when pseudoparticle is affected with a little dissipation of energy, it is trapped in potential well and can oscillate. Oscillations generate shock wave in the media, and in the negative minimal point of the well it is possible to compute numerically the shock wavelength for the allowed values of the plasma parameters.

Type
Papers
Information
Journal of Plasma Physics , Volume 78 , Issue 5 , October 2012 , pp. 525 - 529
Copyright
Copyright © Cambridge University Press 2012

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

[1]Shukla, P. K. 1985 Astrophys. Space Sci. 114, 381.CrossRefGoogle Scholar
[2]Sturrock, P. A. 1971 Astrophys. J. 164, 529.CrossRefGoogle Scholar
[3]Lominadze, J. G., Machabeli, G. Z. and Usov, V. V. 1983 Astrophys. Space Sci. 90, 19.CrossRefGoogle Scholar
[4]Boehmer, H., Adams, M. and Rynn, N. 1995 Phys. Plasmas 2, 4369.CrossRefGoogle Scholar
[5]Liang, E. P., Wilks, S. C. and Tabak, M. 1998 Phys. Rev. Lett. 81, 4887.CrossRefGoogle Scholar
[6]Surko, C. M., Leventhal, M. and Passner, A. 1989 Phys. Rev. Lett. 62, 901.CrossRefGoogle Scholar
[7]Oohara, W. and Hatakeyama, R. 2003 Phys. Rev. Lett. 91, 205005.CrossRefGoogle Scholar
[8]Verheest, F. and Cattaert, T. 2005 Phys. Plasmas 12, 032304.CrossRefGoogle Scholar
[9]Shukla, P. K. and Stenflo, L. 2005 Phys. Plasmas 12, 044503.CrossRefGoogle Scholar
[10]Sagadeev, R. Z. 1966 In Review of Plasma Physics, Vol. 4, pp. 23–91. New York: Consultants Bureau.Google Scholar
[11]Chen, F. F. 1984 Introduction to Plasma Physics and Controlled Fusion, 2nd edn. New York: Plenum.CrossRefGoogle Scholar