14:45 〜 15:00
[PEM17-05] Magnetic Field Amplification by Ion-Weibel Instability in Astrophysical and Laboratory Plasmas
キーワード：宇宙線、超新星残骸、無衝突衝撃波、実験室宇宙物理
It is known that astrophysical shocks accelerate cosmic rays efficiently. Non-relativistic, high Mach number shocks, such as supernova remnants (SNRs), are considered the primary source of galactic cosmic rays. In these shocks, ion-Weibel instability is thought to be the dominant plasma process responsible for magnetic field amplification and shock formation.
Using theory and particle-in-cell (PIC) simulations, we show that a weak but finite background magnetic field (MA~100) plays an essential role in enhanced magnetic field amplification and electron heating compared to unmagnetized (MA>>1000) shocks. This electron heating may be relevant to the electron injection problem.
Although PIC simulation is a powerful tool for understanding plasma microphysics, reduced models in dimension, system size, and electron-to-ion mass ratio are used to save computational resources. We discuss possible laboratory laser experiment setups to verify the theory and simulation. Efficient magnetic field amplification using high-power lasers has applications outside astrophysics, such as medical treatment.
Using theory and particle-in-cell (PIC) simulations, we show that a weak but finite background magnetic field (MA~100) plays an essential role in enhanced magnetic field amplification and electron heating compared to unmagnetized (MA>>1000) shocks. This electron heating may be relevant to the electron injection problem.
Although PIC simulation is a powerful tool for understanding plasma microphysics, reduced models in dimension, system size, and electron-to-ion mass ratio are used to save computational resources. We discuss possible laboratory laser experiment setups to verify the theory and simulation. Efficient magnetic field amplification using high-power lasers has applications outside astrophysics, such as medical treatment.