报告人：季索清　 博士 （UCSB）

时间：2016年1月6日下午4：00

地点：东区理化大楼18层天文台报告厅

报告摘要：Turbulent dynamo field amplification has often been invoked to explain the strong field strengths in thin rims in supernova shocks(~ 100 µG) and in radio relics in galaxy clusters (~ µG). In this talk, we present high resolution MHD simulations of the interaction between pre-shock turbulence, clumping and shocks, to contrast compressional or Richtmyer-Meshov unstable amplification in both situations, and further demonstrate different mechanisms and features of magnetic field amplification between ICM and ISM. Last but not the least, I’ll briefly introduce the yt project (http://yt-project.org) which is a python package for analyzing and visualizing volumetric,
multi-resolution data from astrophysical simulations (such as Enzo,FLASH, Gadget, etc.).