Evolution of nonlinear ion-acoustic solitary wave propagation in rotating plasma

Abstract

A simple unmagnetized plasma rotating around an axis at an angle θ with the propagation direction of the acoustic mode has been taken. The nonlinear wave mode has been derived as an equivalent Sagdeev potential equation. A special procedure, known as the tanh method, has been developed to study the nonlinear wave propagation in plasma dynamics. Further, under small amplitude approximation, the nonlinear plasma acoustic mode has been exploited to study the evolution of soliton propagation in the plasma. The main emphasis has been given to the interaction of Coriolis force on the changes of coherent structure of the soliton. The solitary wave solution finds the different nature of solitons called compressive and rarefactive solitons as well as its explosions or collapses along with soliton dynamics and these have been showing exciting observations in exhibiting a narrow wave packet with the generation of high electric pressure and the growth of high energy which, in turn, yields the phenomena of radiating soliton in dynamics.

Nonlinear Langmuir structures: Soliton and shock in a rotating weakly relativistic electron-positron magnetoplasma with stationary positive ions

“…In fact, the Coriolis force is important in the solar physics involved in sunspot development, the star cycle, and the structure of rotating magnetic stars. 17,18 For example, when a star is transformed into a neutron star, the moment of inertia decreases strongly; thus, the conservation of angular momentum causes a high rotation of the star. Under the condition of frozen in force lines, magnetic flux is also conserved; thus, the field varies in proportion to r −2 ͑r is the radius of the star͒.…”

Dissipative ion acoustic solitary waves in collisional, magneto‐rotating, non‐thermal electron–positron–ion plasma

“…[31] Apart from the well-known Lorentz force creating plasma fluid rotation, Coriolis force is also suggested [32] to be of importance in astrophysical environments. For the case of ummagnetized and rotational plasmas, the authors in refs [34,35] studied the dynamics of arbitrary amplitude non-linear solitary profiles, the first without dust dynamics and the latter with the inclusion of dust dynamics. [33] Due to the important role played by the Coriolis force in rotating space plasma, many researchers have attempted to analyse the wave dynamics in the presence of the Coriolis force.…”

“…[10] By employing the reductive perturbation method, a ZK equation was derived, and the effects of various parameters, like obliqueness, positron concentration, and ion temperature, were discussed on the width and amplitude of solitary waves. For the case of ummagnetized and rotational plasmas, the authors in refs [34,35] studied the dynamics of arbitrary amplitude non-linear solitary profiles, the first without dust dynamics and the latter with the inclusion of dust dynamics. Moslem et al [36] studied the non-linear electrostatic excitations in a magnetized rotating e-p-i plasmas and found that the system supports the propagation of both subsonic and supersonic waves.…”

Instability of electromagnetic waves in a self-gravitating rotating magnetized dusty plasma with opposite polarity grains

“…They have also calculated the equilibrium potential for insulating dust grains immersed in both Maxwellian and generalized Lorentzian plasmas. 25 The rotation rate of planets, in general, is very slow compared to electron and ion timescales. These values may be in the range of the inferred values in different regions of planetary ring systems, comets, interplanetary medium, and supernova remnants.…”