  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.
