Two-Dimensional MHD Simulation of Quasi-Spherical and Cylindrical Metallic Liner Acceleration

Abstract

model, based upon the Lindemann melting law, will be used later. We have performed 2D lagrangian MHD simulations for HEL and quasi-spherical liner systems in a Z-pinch configuration. For the HEL system, we have obtained II.COMPUTATIONAL DETAILS reasonable agreement with the experimental values of liner velocity, kinetic energy and the liner shape.We have performed computer simulations for two In quasi-spherical liner system simulation, there is a experimental systems, details of which are available in the good match with published results for the liner shape and literature. These are the High Energy Liner (HEL) [3] and radius until t = 12.7 gs. Also, our simulation indicates the quasi-spherical liner acceleration [4] experiments. melting, but no vaporization, as reported in the literature. Details are given in the following sub-sections.However, as convergence proceeds toward the axis, we find large distortions in the inner surface of the liner, A. High Energy Liner (HEL) system which do not allow the simulation to continue beyondThe HEL system [3] consists of a thin cylindrical shell 14.4 gs. This is a major mismatch with 2D MHD made of aluminum, having a thickness of 4 mm. It has an simulations reported in the literature.initial outer radius of 240 mm and a length of 100 mm.

Comparison of Magnetohydrodynamics Simulation And Observasional Result to Solar Coronal Helmet Streamer

“…The only way for validation with real physical world is accomplished through density output from computation with the density provided from observational data, since the helmet streamer from real corona is nothing than the electron density scattered by Thomson electron scattering mechanism. The formula to convert from intensity data to density data is written as [7] …”

“…Magnetohydrodynamics transport equation used to study process the helmet streamer formation [4,6,7]. The equations is Mass transport:…”

“…We solve in a way such that the solution has second order accuracy in space and in time. Adiabatic environment (γ = 5/3) is assumed during the helmet streamer formation [7,9]. The plasma pressure P and plasma density ρ are directly computed through equations (1) and (4), while the plasma temperature T is derived from equation (5).…”

“…The bottom boundary is hard boundary which makes the coronal magnetic fields in line-tied condition. The plasma can penetrate the bottom boundary from below as a result of ever escaping plasma from the photosphere and the chromospheres [6,7,9].…”

“…The idea of research is magnetic fields can induce currents in a moving conductive fluid, which create forces on the fluid. The set of equations which describe this condition are combination of the NavierStokes equations of fluid dynamics and Maxwell's equations of electromagnetism [3,6,7]. Magnetohydrodynamics equation was used in reference to the transfer of momentum from the Sun to the planets, but it's eventually expanded upon to include the current field.…”