Analysis of radiative gravitational modes in magnetized dusty plasma with non-thermal ion distribution

Abstract

The characteristics of radiative gravitational modes in non-thermal magnetized dusty plasma with charge fluctuation and the polarization force of dust particles are investigated. The electron species are assumed to be radiative and the ions are assumed to be non-thermal. A normal mode analysis is applied to derive the general dispersion relation for radiative magnetized selfgravitating dusty plasma. Modified radiative condensation and self-gravitational instability criteria for both perpendicular and parallel modes of propagation are obtained. Analytically, it is found that the presence of a non-thermal ion population significantly modified the usual radiative condensation instability criterion, and damped the growth rate of the radiative mode. The obtained analytical results are further discussed in the numerical result section. We investigate the fact that the non-thermal ion population acts as a stabilizing source for radiative condensation instability in magnetized self-gravitating dusty plasma fluid, including the dust polarization force and charge fluctuation. The thermal conductivity with non-thermal ion distribution quickly moves the system towards stability. The implications of the results in the region of the interstellar medium (ISM) are discussed.

Influence of ionization and ion loss on radiative and gravitational instabilities of inhomogeneous plasma with dust polarization force

“…Thus, the present work is the modification of the previous work done by Prajapati et al [37]. In absence of recombination frequency, ion streaming velocity and neutral effects from equation (24) then the obtained dispersion relation is similar to the dispersion relation obtained by Patidar et al [38] ignoring magnetic field and non-thermal ion distribution from that case.…”

“…We numerically analyze the dispersion relation (25) to see how the ionization, recombination, polarization force, neutral dynamics and dust thermal velocity modify the growth rate of instabilities. For the numerical estimation, equation (25) is written in dimensionless form as For numerical calculations we have chosen the typical plasma parameters from [34,38,40,41] which are found in various astrophysical dusty plasma situations. In order to analyze the effects of various parameters on the growth rate of instabilities, we have plotted the real positive values of dimensionless growth rate of equation (34) versus the normalized wave number.…”