Theoretical Treatment of Drift Waves in A Collisionless Plasma Regime

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A theoretical model is introduced in this study which is based on two-fluid equations, for either electrons or ions and simplified to the collisionless magnetised plasma regime. In the present work, that the inclusion of electron temperature gradient is essential and must be taken into account in the theory. In addition, the E ×B plasma rotation which arises when a radial electric field exist in an axial magnetic field is included into a theoretical model. The effect of rotation will Doppler shift the drift wave frequency so that plasma rotates as a solid body. The radial plasma density and temperature profiles which are required as input to the theoretical calculation are also presented and displayed. The theoretical model predicts the actual frequency, and the radial fluctuation profiles of the mode and hence, the position of the maximum wave amplitude can be determined. We made a comparison of experimental measurement with the theoretical prediction for radial variation of eigen function of density fluctuation are also presented. The experimental data is obtained from an axial magnetised plasma of Zhang L. (1992) results.

Autorentext

  • Associate Research Assistant at Center for Astronomy and Space Sciences, Al Aqsa University. Author of Introduction to Astronomy in Arabic ( ).Editor of Eyes to Sky astronomical Journal now three editions are published. Member of the Palestinian Amateur Astronomy club-Gaza. Member of Aura Physics Society-Gaza.

Weitere Informationen

  • Allgemeine Informationen
    • GTIN 09783330854321
    • Genre Physics
    • Anzahl Seiten 84
    • Herausgeber Noor Publishing
    • Größe H220mm x B150mm
    • Jahr 2017
    • EAN 9783330854321
    • Format Kartonierter Einband
    • ISBN 978-3-330-85432-1
    • Veröffentlichung 04.04.2017
    • Titel Theoretical Treatment of Drift Waves in A Collisionless Plasma Regime
    • Autor Soboh Alqeeq
    • Untertitel Within A Magnetically Confined Plasma
    • Sprache Englisch

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