Non-planar magnetoactive GES-based solar plasma stability

TL;DR

This paper develops a non-planar GES-based model to analyze the stability of magnetoactive solar plasma systems, revealing the influence of magnetic fields, density, and temperature on plasma stability and wave behavior.

Contribution

It introduces a novel non-planar GES formalism for solar plasma stability analysis, extending previous plane-wave models to spherical geometries with turbulence effects.

Findings

Stability depends mainly on magnetic field, density, and temperature.

Dispersive features are more prominent in self-gravitational domains.

Magneto-thermal effects can both stabilize and destabilize plasma modes.

Abstract

A laboratory plasma-wall interaction-based astrophysical gravito-electrostatic sheath (GES) model is methodologically applied to study the dynamic stability of the magnetoactive bi-fluidic solar plasma system in the presence of turbulence effect. The spherically symmetric GES-model formalism couples the solar interior plasma (SIP, internally self-gravitating, bounded) and the solar wind plasma (SWP, externally point-gravitating, unbounded) through the diffused solar surface boundary (SSB). A normal spherical mode ansatz results in a generalized linear quadratic dispersion relation depicting the modal fluctuations on both the SIP and SWP scales. A constructive numerical platform reveals the evolution of both dispersive and non-dispersive modal features of the modified-GES mode excitations. The reliability of the derived non-planar dispersion laws is concretized with the help of an exact analytic shape matching the previously reported results founded on the plane-wave approximation. It is found that the thermo-statistical GES stability depends mainly on the magnetic field, equilibrium plasma density, and plasma temperature. It is speculated that the dispersive features are more pronounced in the self-gravitational domains against the electrostatic ones. The magneto-thermal interplay introduces decelerating (accelerating) and destabilizing (stabilizing) influences on the SIP (SWP), and so forth. At last, we briefly indicate the applicability of the proposed analysis to understand diverse helioseismic activities from the collective plasma dynamical viewpoint in accordance with the recent astronomical observational scenarios reported in the literature.