Nonlinear Self‐Gravitational Solar Plasma Fluctuations with Electron Inertia

Karmakar, Pralay Kumar; Borah, B.

doi:10.1002/ctpp.201200132

Cited by 5 publications

(2 citation statements)

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“…So, a numerical illustrative scheme is developed on the basis of the fourth-order Runge-Kutta (RK-IV) method [6,12]. It employs all the reliable input and initial data of real astronomical relevance available as widely employed in the literature for the solar plasma description [1,2,[13][14][15]18,19,21]. The results thus obtained via simulation are pictorially illustrated in figs.…”

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confidence: 99%

“…The normalized standard set of the basic governing equations consists of the equation of continuity for the ionic flux-density conservation, momentum equation for the ionic force-density conservation, heat-flow equation for the net thermal energy conservation, and the gravitational Poisson equation for the material density-potential field coupling [12][13][14][15][16][17][18][19][20][21]. Applying eq.…”

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An elog-KdVB dynamics in non-thermal solar plasmas

Karmakar¹,

Kashyap²

2018

EPL

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This paper deals with a continued study on the basis of the gravito-electrostatic sheath (GES) model to explore the excitation of solitary and shock-like wave structures evolving in the non-thermal solar plasmas. The method applied here is based on a nonlinear local perturbation analysis over the GES structure equations designed in a thermostatistically modified form to arrive at an extended logatropic Korteweg-de Vries-Burgers (elog-KdVB) equation with a unique linear derivative source, which has in principle, a special set of multiparametric coefficients dependent on the diversified solar plasma parameters. A constructive numerical integration of the elog-KdVB equation yields the excitation of rarefactive shock-like wave patterns supported in the solar plasmas. Their noticeable unique characteristic feature is the naturalistic existence of distorted non-uniform tails. The shock-wave amplitude increases with the increase in the thermostatistical power (κ), and vice versa. In contrast, the shock-tail width decreases with the increase in the thermostatistical distribution power (κ), and vice versa. It implicates that the shock-tail width vanishes in the Boltzmann thermostatistical limit (κ → ∞). The corresponding gradients, phase portraits, and curvature dynamics associated with the fluctuations are illustratively depicted. The microphysical details behind the dynamics are analyzed. The elog-KdVB dynamical results explored are bolstered with the reinforcement of the earlier multispace satellitic observations and original probe measurements reported elsewhere. The non-trivial implications and applications are summarily highlighted in the real helioseismic contextual linkage.

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