Speaker
Description
A low-$\beta$ plasma is characterized by a dominance of magnetic energy over internal (kinetic) energy, where the magnetic pressure ($B^2/2\mu_0$) surpasses the kinetic pressure ($p$), confining the plasma within magnetic fields. Under specific conditions, low-$\beta$ plasmas adhere to Alfvén's theorem, wherein magnetic field lines remain 'frozen' within the plasma and move with it. These plasmas are commonly associated with magnetic confinement fusion reactors, star atmospheres, and plasma-based space propulsion technologies.
This talk aims to present findings from plasma acceleration simulations conducted using magnetohydrodynamics (MHD) and Particle-In-Cell (PIC) codes. The study will review Weber-Davis solar wind acceleration, following Parker's theoretical framework. Furthermore, various plasma acceleration modes have been studied, including the critical points responsible for accelerating solar winds from subsonic to supersonic velocities. Transitioning from solar winds to magnetic nozzle scenarios involves minor adjustments, leading to a convergent-divergent magnetic field configuration that converts plasma's thermal energy into directed kinetic energy.
Both PIC and MHD simulations are analyzed and compared to understand plasma acceleration modes, with a focus on torsional Alfvén waves, pressure-induced acceleration, and centrifugal confinement.
| Keyword-1 | Plasma acceleration |
|---|---|
| Keyword-2 | Low-beta plasmas |
| Keyword-3 | Magnetohydrodynamics |
