标题： 磁化星际介质中超新星遗迹的长期演化 显示英文标题

标题： Long-Term Evolution of Supernova Remnants in Magnetized Interstellar Medium

摘要： 研究了超新星遗迹（SNRs）的演化，特别关注了轴对称二维磁流体力学模拟中磁场的影响。 在绝热Sedov阶段，磁场SNRs的演化与无磁场的SNRs相同。 当薄壳形成后，壳层由热内部气体（气泡）的压力驱动。 压力驱动的雪犁阶段的演化受到磁场的显著影响。 由于磁压效应，扫过磁场线的壳层变厚。 从$5\times 10^5{\rm yr}$到$2\times 10^6{\rm yr}$后，厚壳内边界开始收缩。 这使热气泡径向压缩并维持其热压。 因此，气泡形成一个长椭球形状，并因沿磁场方向扩展而变得越来越薄，直至$B_0 \gtrsim 3\mu {\rm G}$。 最终，气泡收缩。 考虑到磁场的作用，星际介质中热低密度气体的孔隙度降低。 显示英文摘要

摘要： The evolution of supernova remnants (SNRs) is studied, with particular attention to the effect of magnetic fields with axisymmetric two-dimensional magnetohydrodynamical simulations. The evolution of magnetic SNRs is the same as non-magnetic ones in the adiabatic Sedov stage. After a thin shell is formed, the shell is driven by the pressure of the hot interior gas (bubble). Evolution in the pressure-driven snow-plow phase is much affected by the magnetic field. The shell sweeping the magnetic field lines thickens owing to the magnetic pressure force. After $5\times 10^5{\rm yr}$ - $2\times 10^6{\rm yr}$, the inner boundary of the thick shell begins to contract. This compresses the hot bubble radially and maintains its thermal pressure. Thus, the bubble forms a prolate spheroidal shape and becomes thinner and thinner, since it expands in a direction parallel to the magnetic field for $B_0 \gtrsim 3\mu {\rm G}$. Finally, the bubble contracts. The porosity of the hot low-density gas in ISM is reduced, taking the effect of the magnetic field into account.