Nonlinear Korteweg-de Vries-Burger equation for ion acoustic shock waves in a weakly relativistic electron-positron-ion plasma with thermal ions

Details Nonlinear Korteweg-de Vries-Burger equation for ion acoustic shock waves in a weakly relativistic electron-positron-ion plasma with thermal ions Nonlinear Korteweg-de Vries-Burger equation for ion acoustic shock waves in a weakly relativistic electron-positron-ion plasma with thermal ions

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010phpl...17c2308s&link_type=abstract

Physics of Plasmas, Volume 17, Issue 3, pp. 032308-032308-8 (2010).

Physics

12

Astrophysical Plasma, Convection, Plasma Ion Acoustic Waves, Plasma Shock Waves, Plasma Temperature, Pulsars, Relativistic Plasmas, Stellar Atmospheres, Shock Waves And Discontinuities, Relativistic Plasmas, Plasma Properties, Pulsars, Electrostatic Waves And Oscillations, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation

Scientific paper

The nonlinear propagation of ion acoustic waves in electron-positron-ion plasma comprising of Boltzmannian electrons, positrons, and relativistic thermal ions has been examined. The Korteweg-de Vries-Burger equation has been derived by reductive perturbation technique, and its shock like solution is determined analytically through tangent hyperbolic method. The effect of various plasma parameters on strength and structure of shock wave is investigated. The pert graphical view of the results has been presented for illustration. It is observed that strength and steepness of the shock wave enervate with an increase in the ion temperature, relativistic streaming factor, positron concentrations, electron temperature and they accrue with an increase in coefficient of kinematic viscosity. The convective, dispersive, and dissipative properties of the plasma are also discussed. It is determined that the electron temperature has remarkable influence on the propagation and structure of nonlinear wave in such relativistic plasmas. The numerical analysis has been done based on the typical numerical data from a pulsar magnetosphere.

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