A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability
arXiv:2403.14182 · doi:10.1093/mnras/stad1664
Abstract
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.
arXiv comment26 pages, 28 figures, 6 tables
References in corpus (28)
- Helioseismology
- Eddington's theory of gravity and its progeny
- Probing the interior physics of stars through asteroseismology
- Compact stars in Eddington inspired gravity
- Asteroseismology of solar-type stars
- Magnetic Reconnection as the Driver of the Solar Wind
- The evolution of the solar wind
- A model of acceleration of Anomalous Cosmic Rays by Reconnection in the Heliosheath
- Testing alternative theories of gravity using the Sun
- Nonextensivity and the power-law distributions for the systems with self-gravitating long-range interactions
- The role of torsional Alfven waves in coronal heating
- Generic magnetic field intensity profiles of interplanetary coronal mass ejections at Mercury, Venus and Earth from superposed epoch analyses
- Solar inertial modes: Observations, identification, and diagnostic promise
- Does Turbulent Pressure Behave as a Logatrope?
- The Generation of Coronal Loop Waves below the Photosphere by p-Mode Forcing
- The effects of plasma beta and anisotropy instabilities on the dynamics of reconnecting magnetic fields in the heliosheath
- Experimental Observation of Electron-Acoustic Wave Propagation in Laboratory Plasma
- The effect of magnetic field on the damping of slow waves in the solar corona
- What does the nonextensive parameter q stand for in self-gravitating systems ?
- SWASTi-SW: Space Weather Adaptive SimulaTion framework for Solar Wind and its relevance to ADITYA-L1 mission
- Origin of Multifractality in Solar Wind Turbulence: the Role of Current Sheets
- A spectral solver for solar inertial waves
- Dependence of sunspot photospheric waves on the depth of the source of solar modes
- Acceleration of Solar Energetic Particles by the shock of Interplanetary Coronal Mass Ejection
- Imaging the Sun's near-surface flows using mode-coupling analysis
- Modified Gravity at Astrophysical Scales
- The next generation Birmingham Solar Oscillations Network (BiSON) spectrophotometer: a new miniaturised instrument for helioseismology
- Non-planar magnetoactive GES-based solar plasma stability