Description
Plethora of naturalistic waves and oscillations are ubiquitous in the entire solar plasma spatiotemporal regime. A linear perturbative analysis is methodically performed to study the stability dynamics of the nonthermal viscoturbulent inhomogeneous solar plasmas. The fluid turbulence effects are included with the Larson logabarotropic equation of state. The suprathermal lighter species (electrons) are modelled with the generalised $(r, q)$-distribution law. Diversified characteristics of the helioseismic collective waves and oscillations are investigated. The effect of low-energetic (governed by spectral index $r$) and high-energetic (governed by spectral index $q$) electrons on the fluctuation behaviour of g-mode and p-mode is analyzed and characterized extensively. A linear normal mode treatment yields a unique pair of cubic dispersion relations describing the bounded solar interior plasma (SIP, self-gravity) and the unbounded solar wind plasma (SWP, external gravity). The non-trivial effect of the nonthermality indices ($r$ and $q$), solar electron tem perature, plasma dynamic viscosity, and thermal conductivity on the dispersion signatures is elaborately explored. The p-mode propagates throughout the Sun and its outer atmosphere. The g-mode dominates only inside the deeper layers. The excitation of solar five-minute oscillations is theoretically analysed and observationally confirmed. The electron nonthermality, temperature, and thermal conductivity play mode-accelerating roles against the viscosity. The radially outward photospheric p-mode energy flux is estimated analytically as $10^3-10^5$ W m$^{-2}$. It is demonstrated that these p-modes contribute significantly to chromospheric spicule formation through longitudinal-to-transverse mode conversion processes. Finally, manifold helioseismic observations from the literature fairly bolster our proposed model reliability.
