Jeans instability analysis of viscoelastic astrofluids in Eddington-Inspired-Born–Infeld(EiBI) gravity

Yang, Qiaoyun; Tan, Ling; Chen, Hui; Liu, Sanqiu

doi:10.1016/j.newast.2022.101947

Cited by 13 publications

(1 citation statement)

References 48 publications

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“…It immensely affects the evolution and the equilibrium structure of the self-gravitating sun and provides modified core temperature and acoustic mode profiles (Casanellas et al 2012 ). In this context, the modern formulation of Eddington-inspired-Born-Infeld (EiBI) theory is e xtensiv ely e xplored to present no v el modified gravitational description of selfgravitating astrophysical spatiotemporal scales, such as the solar interior structure (Ba ˜ nados & Ferreira 2010 ;Casanellas et al 2012 ;Yang et al 2023 ). Thus, in our solar plasma model, the EiBI theory could be taken fruitfully to explain solar plasma dynamics in the light of the post-Newtonian formalism of modern gravitational scenario.…”

Section: O N C L U S I O N Smentioning

confidence: 99%

A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability

DAS

Atteya

Karmakar

2023

Monthly Notices of the Royal Astronomical Society

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A recently reported Gravito-Electrostatic Sheath (GES) model is procedurally applied to study the turbumagnetoactive helioseismic oscillation features in the entire bi-fluidic solar plasma system (DAS & KARMAKAR, JOAA, 2022). 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 counterparts (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, SolO, etc.

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Section: O N C L U S I O N Smentioning

confidence: 99%

A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability

DAS

Atteya

Karmakar

2023

Monthly Notices of the Royal Astronomical Society

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Magnetogravitational instability in strongly coupled rotating clumpy molecular clouds including heating and cooling functions

Dhiman,

Mahajan

2023

Astrophys Space Sci

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The molecular clouds (MCs) formation is caused due to gravitational collapse mechanism and is significantly affected due to radiative heating and cooling processes. The paper analyzes the gravitational instability in the strongly coupled clumpy MCs, under the effects of uniform rotation, magnetic field, and heatloss functions. The generalized hydrodynamic (GHD) equations coupled with the modified energy equation (which incorporates the heating and cooling effects due to cloud-cloud collisions) are used to describe the mathematical model. A general dispersion relation is analytically derived using the normal mode analysis method, by taking the orientations of the magnetic field and uniform rotation along the vertical direction. The Jeans criteria of gravitational instability are obtained for strongly and weakly coupling limits, which are modified due to the Coulomb coupling parameter, heat-loss functions, and viscoelastic coefficients. It is found that the value of the critical wavenumber decreases due to the strong coupling between the plasma particles (coupling parameter) and clump stirring processes (heating rate), thus both have stabilizing influence on the onset of gravitational collapse in clumpy MCs. The influence of various parameters on the growth rate of the instability is discussed numerically and it is found that the cooling rate parameter which described the cloud-cloud collisions shows the destabilizing effect. The region of instability is observed to be smaller in the strongly coupled clumps (kinetic limit) than in the weakly coupled (hydrodynamic limit) clumps. The results are helpful in understanding the role of heating and cooling mechanisms in the MCs formation.

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Dynamics of pulsational mode in the EiBI gravity fabric

Das,

Karmakar

2024

Chinese Journal of Physics

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Jeans instability analysis of viscoelastic astrofluids in Eddington-Inspired-Born–Infeld(EiBI) gravity

Cited by 13 publications

References 48 publications

A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability

A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability

Magnetogravitational instability in strongly coupled rotating clumpy molecular clouds including heating and cooling functions

Dynamics of pulsational mode in the EiBI gravity fabric

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