首页|Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants
Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants
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Using an effective adiabatic index γeff to mimic the feedback of efficient shock acceleration,we simulate the temporal evolution of a young type Ia supemova 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 γeff 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 γeff=1.1,they are amplified about 10-26 times more than those with γeff=5/3.While in the angular direction,the total magnetic energy densities could be amplified about 350 times more than those with γeff=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.
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