Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants  

作　　者：Jun-Yu Shen Bi-Wen Bao Li Zhang 

机构地区：[1]Department of Astronomy,Key Laboratory of Astroparticle Physics of Yunnan Province,Yunnan University,Kunming 650091,China [2]Key Laboratory of Statistical Modeling and Data Analysis of Yunnan Province,Yunnan University,Kunming 650091,China

出　　处：《Research in Astronomy and Astrophysics》2024年第6期234-244,共11页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China 12233006;partially supported by the National Natural Science Foundation of China 12203042;the Foundations of Yunnan Province 202301AU070009。

摘　　要：Using an effective adiabatic index γ_(eff) to mimic the feedback of efficient shock acceleration,we simulate the temporal evolution of a young type Ia supernova remnant (SNR) with two different background magnetic field(BMF) topologies:a uniform and a turbulent BMF.The density distribution and magnetic-field characteristics of our benchmark SNR are studied with two-dimensional cylindrical magnetohydrodynamic simulations.When γ_(eff)is considered,we find that:(1) the two-shock structure shrinks and the downstream magnetic-field orientation is dominated by the Rayleigh–Taylor instability structures;(2) there exists more quasi-radial magnetic fields inside the shocked region;and (3) inside the intershock region,both the quasi-radial magnetic energy density and the total magnetic energy density are enhanced:in the radial direction,with γ_(eff)=1.1,they are amplified about 10–26 times more than those with γ_(eff)=5/3.While in the angular direction,the total magnetic energy densities could be amplified about 350 times more than those with γ_(eff)=5/3,and there are more grid cells within the intershock region where the magnetic energy density is amplified by a factor greater than 100.

关 键 词：methods:numerical ISM:magnetic fields ISM:supernova remnants magnetohydrodynamics(MHD) 

分 类 号：P145.3[天文地球—天体物理]