Abstract
A nonextensive nonthermal magnetized viscoelastic astrofluid, compositionally containing nonthermal electrons and ions together with massive polarized dust micro-spherical grains of variable electric charge, is allowed to endure weakly nonlinear perturbation around its equilibrium. The nonextensivity originating from the large-scale non-local effects is included via the Tsallis thermo-statistical distribution laws describing the lighter species. Assuming the equilibrium as a homogeneous hydrostatic one, the dust polarization effects are incorporated via the conventional homogeneous polarization force law. The perturbed fluid model evolves as a unique conjugate pair of coupled extended Korteweg-de Vries (e-KdV) equations. A constructed numerical tapestry shows the collective excitations of a new pair of distinct classes of nonlinear mode structures in new parametric space. The first family indicates periodic electrostatic compressive eigenmodes in the form of soliton-chains. Likewise, the second one reveals gravitational rarefactive solitary patterns. Their microphysical multi-parametric dependencies of the eigen-patterns are illustratively analyzed and bolstered. The paper ends up with some promising implications and applications in the astro-cosmo-plasmic context of wave-induced accretive triggering processes responsible for gravitationally bounded (gravito-condensed) astro-structure formation, such as stellesimals, planetsimals, etc.
Highlights
The self-gravitating complex astrofluids in interstellar media exhibit the excitation of wide-range spectra of collective waves, instabilities and oscillations fundamentally responsible for diversified material transport processes leading to building up of early phase of bounded structure formation in diversified astro-cosmic environs.[1,2,3]
A weakly nonlinear perturbation analysis is carried out to derive a conjugate pair of coupled extended Korteweg-de Vries (e-Korteweg-de Vries (KdV)) equations (Eqs. (22), (24)) for a charged cloud stability analysis with the source at the GEM origin
The time-stationary patterns are exhibited in Figs.[1,2,3] for the electrostatic case, Figs. 5–6 for the gravitational one; and the spatiotemporal features are in Fig. 4 and Fig. 7, respectively
Summary
The self-gravitating complex astrofluids in interstellar media exhibit the excitation of wide-range spectra of collective waves, instabilities and oscillations fundamentally responsible for diversified material transport processes leading to building up of early phase of bounded structure formation in diversified astro-cosmic environs.[1,2,3] A number of researchers have studied the basic excitation tenets of such collective wave-kinetic processes in different frameworks in this direction in the past. It may be clearly noted that understanding the complex dynamics of various nonlinear wave excitation processes in a vast nonthermal inhomogeneous astrocloud in the conjoint action of nonlocality-induced nonextensivity, viscoelasticity and polarized dust-charge variation has still been remaining an open thematic problem to be well investigated, explored and enlightened. We report on a new theoretic evolutionary model development to study the propagatory dynamics of weakly nonlinear behaviour of gravito-electro-magnetic (GEM) fluctuations in self-gravitating viscoelastic magnetized nonthermal complex grainy astroplasmas in the presence of polarized dust-charge variation dynamics for the first time to the best of our knowledge. The dust polarization force originates from the interaction of the thermal electron-ion currents over the grain surfaces in a random erratic fashion.[3] The thermal species thermostatistically obey nonextensive distribution laws since they are out of thermal equilibrium due to the large-scale inherent gradient and inhomogeneity forces. The results are compared with the existing analytic scenarios together with promising indications to non-trivial applicability in the astro-space-cosmic context of bounded structure formation in dynamic cloud collapse mechanisms triggered by waveinduced fluid accretions
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