中心能量注入下柱面磁流体动力学爆炸波的自相似解
Self-similar solutions in cylindrical magneto-hydrodynamic blast waves with energy injection at the centre
AI总结：
本文研究了中心源驱动的柱面磁化爆炸波在方位角和轴向环境磁场下的自相似解，发现磁场取向显著影响激波速度、壳层厚度及能量转化，并通过1D数值模拟验证了模型在星风泡和超新星遗迹中的适用性。
摘要：
大质量恒星驱动的激波演化不仅取决于周围磁场强度，还与其方向有关。本文研究了在方位角和轴向环境磁场共同影响下，磁化爆炸波的动力学行为。该爆炸波由中心源驱动，并形成一个由激波后方星际物质堆积而成的壳层。通过假设环境磁场的相似形式和爆炸波的柱面几何结构，获得了自相似解。模型分别针对方位角和轴向磁场进行了研究，并利用1D数值模拟分别应用于星风泡和超新星遗迹。研究发现，磁化爆炸波与无环境磁场的自相似情况不同。在方位角情况下，前向激波前沿速度较慢，而在轴向情况下则较快。对于两种切向取向，壳层的厚度均随磁场强度增加而增加。在方位角情况下，热能可以在壳层内边界附近转化为磁能。因此，星风泡的切向不连续面处温度下降，磁场增强。在超新星遗迹的轴向情况下，数值解始终遵循自相似模型给出的参数空间中的特定曲线。
英文摘要：
The evolution of shocks induced by massive stars does not depend only on the ambient magnetic field strength, but also on its orientation. In the present work, the dynamics of a magnetized blast wave is investigated under the influence of both azimuthal and axial ambient magnetic fields. The blast wave is driven by a central source and forms a shell that results from the accumulation of interstellar matter behind the shock front. A similarity form of the ambient magnetic field and a cylindrical geometry of the blast wave are assumed to obtain self-similar solutions. The model is studied separately for both azimuthal and axial magnetic field and applied to stellar wind bubbles and supernova remnants respectively, using 1D numerical simulations. We found that the magnetized blast wave differs from the self-similar case without an ambient magnetic field. The forward shock front goes slower in the azimuthal case and faster in the axial one. For both tangential orientations, the thickness of the shell increases with the magnetic strength. In the azimuthal case, the thermal energy can be converted to magnetic energy near the inner boundary of the shell. Thus, the temperature drops and the magnetic field increases at the tangential discontinuity of the stellar wind bubble. In the axial case of a supernova remnant, the numerical solution al w ays follows a special curve in the parameter space given by the self-similar model.
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