Volume 124, Number 3, November 2018
|Number of page(s)
|Geophysics, Astronomy and Astrophysics
|06 December 2018
An elog-KdVB dynamics in non-thermal solar plasmas
Department of Physics, Tezpur University - Napaam-784028, Tezpur, Assam, India
Received: 2 May 2018
Accepted: 30 October 2018
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 (). 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.
PACS: 95.30.Qd – Magnetohydrodynamics and plasmas / 96.60.-j – Solar physics / 96.60.Jw – Solar interior
© EPLA, 2018
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