Pulsational mode stability in complex EiBI-gravitating polarized astroclouds with (r, q)-distributed electrons

TL;DR

This paper investigates how EiBI gravity, non-thermal electron distributions, and dust polarization influence the stability of pulsational modes in complex astrophysical clouds, revealing factors that can trigger or prevent collapse.

Contribution

It introduces a semi-analytic model combining EiBI gravity, non-thermal electron distributions, and dust polarization effects on pulsational mode stability in astrophysical clouds.

Findings

Polarization force and positive EiBI parameter increase instability.

Electron non-thermality parameters stabilize the cloud.

Results align with previous astronomical predictions.

Abstract

The pulsational mode of gravitational collapse (PMGC) originating from the combined gravito-electrostatic interaction in complex dust molecular clouds (DMCs) is a canonical mechanism leading to the onset of astronomical structure formation dynamics. A generalized semi-analytic model is formulated to explore the effects of the Eddington-inspired Born-Infeld (EiBI) gravity, non-thermal (r, q)-distributed electrons, and dust-polarization force on the PMGC stability concurrently. The thermal ions are treated thermo-statistically with the Maxwellian distribution law and the non-thermal electrons with the (r, q)-distribution law. The constitutive partially ionized dust grains are modeled in the fluid fabric. A spherical normal mode analysis yields a generalized linear PMGC dispersion relation. Its oscillatory and propagation characteristics are investigated in a reasonable numerical platform. It is found that an increase in the polarization force and positive EiBI parameter significantly enhances the instability, causing the DMC collapse and vice versa. The electron non-thermality spectral parameters play as vital stabilizing factors, and so on. Its reliability and applicability are finally outlined in light of astronomical predictions previously reported in the literature.