Volume 121, Number 3, February 2018
|Number of page(s)||5|
|Section||Physics of Gases, Plasmas and Electric Discharges|
|Published online||29 March 2018|
A non-ideal MHD model for structure formation
Department of Physics, Tezpur University - Napaam-784028, Tezpur, Assam, India
Received: 11 January 2018
Accepted: 5 March 2018
The evolutionary initiation dynamics of triggered planetary structure formation is indeed a complex process yet to be well understood. We herein develop a theoretical classical model to see the gravitational fragmentation kinetics of the viscoelastic non-ideal magneto-hydro-dynamic (MHD) fabric. The inhomogeneous planetary disk is primarily composed of heavier dust grains (strongly correlated) together with relatively lighter electrons, ions and neutrals (weakly correlated) in a mean-fluidic approximation. A normal harmonic mode analysis results in a quadratic dispersion relation of a unique shape. It is demonstrated that the growth rate of the MHD fluctuations (magnetosonic) contributing to the planet formation rate, apart from the wave vector and its projection orientation, has a pure explicit dependency on the viscoelastic parameters. The analysis specifically shows that the effective generalized viscosity , viscoelastic relaxation time , and K-orientation play as destabilizing agencies against the non-local gravitational disk collapse. The relevancy is briefly indicated in the real astronomical context of bounded planetary structure formation and evolution.
PACS: 52.27.Lw – Dusty or complex plasmas; plasma crystals / 04.40.-b – Self-gravitating systems; continuous media and classical fields in curved spacetime / 95.30.Lz – Hydrodynamics
© EPLA, 2018
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