  A recently reported gravito-electrostatic sheath (GES) model is procedurally
applied to study the turbumagnetoactive helioseismic oscillation features on
the entire bi-fluidic solar plasma system. The bounded solar interior plasma
(SIP, internally self-gravitating) and the unbounded solar wind plasma (SWP,
externally point-gravitating) are coupled through the interfacial diffused
solar surface boundary (SSB) due to an exact gravito-electrostatic interplay. A
numerical platform on the developed theoretic formalism reveals the evolution
of both dispersive and non-dispersive features of the modified GES mode
fluctuations in new parametric windows. Different colourspectral profiles
exhibit important features of the GES-based SIP-SWP perturbations elaborately.
It is illustratively shown that the thermostatistical GES stability depends
mainly on the radial distance, magnetic field, equilibrium plasma density, and
plasma temperature. We see that their dispersive features are more pertinently
pronounced in the self-gravitational domains (SIP) than the electrostatic ones
(SWP). Besides, different characteristic parameters with accelerating (or
decelerating) and stabilizing (or destabilizing) effects influencing the entire
solar plasma stability are illustratively portrayed. We speculate that, in the
SIP, the long-wave (gravitational-like) helioseismic fluctuations become highly
dispersive showing more propagatory nature than the shorter ones
(acoustic-like). The short waves show more propagatory propensity than the
longer ones in the SSB and SWP regime. The reliability of our proposed
investigation is bolstered along with the tentative applicability and future
scope in light of the current solar observational scenarios, such as SOHO,
STEREO, SDO, PSP, and SolO.
