Athermal GES-based solar plasma stability with sphero-logabarotropic special effects

¹ Department of Physics, Tezpur University - Napaam-784028, Tezpur, Assam, India
² Department of Physics, Manipal Institute of Technology Bengaluru, Manipal Academy of Higher Education Manipal, India
³ Department of Physics, Sikkim Manipal Institute of Technology, Sikkim Manipal University Majitar, East Sikkim, Sikkim-737136, India

^(a) pkk@tezu.ernet.in (corresponding author)
^(b) deka.utpal@manipal.edu

Received: 2 January 2022
Accepted: 27 June 2022

Abstract

A model formalism for the small-scale radial fluctuations excitable in the athermal (non-thermal) solar plasma system on the basis of the non-extensive gravito-electrostatic sheath (GES) model fabric is reported. A unique speciality here is that it intercouples the solar interior plasma (SIP) and the solar wind plasma (SWP) gravito-electrostatically via the interfacial diffused solar surface boundary (SSB). The constitutive electrons are thermostatistically framed in the κ-distribution laws via the Tsallis thermostatistics. In contrast, the heavier ions are treated as an inhomogeneous fluid. The turbulent degrees of freedom are accounted through the Larson nonlinear logabarotropic equation of state in curved geometry. A spherically symmetric wave analysis over the perturbed GES structure results in a unique pair of distinct linear dispersion laws (SIP plus SWP) without any typical quasi-classic approximation. A numerical illustrative platform for the dispersion analysis specifically shows that an antikink-type (kink-type) impulsive rarefactive (compressive) propagatory boost due to irregular dispersion is experienced by the fluctuations at the heliospheric core (photospheric SSB). We see that the thermostatistical parameter (Tsallis power-law tail index κ) acts as a unique form of acceleration agency for both the SIP and SWP instabilities to proliferate. At the last, the explorative semi-analytic results are contextually compared with the realistic domains of the collective excitation of the helioseismic waves and SSB oscillations.