蜗牛的射电偏振观测：G327 .1-1.1中具有高度有序磁场的破碎脉冲星风星云
Radio Polarization Observations of the Snail: A Crushed Pulsar Wind Nebula in G327.1-1.1 with a Highly Ordered Magnetic Field
摘要：
脉冲星风星云（PWNe）被认为是银河系中宇宙射线的加速场。虽然磁场在加速过程中起着重要的作用，以前的观测磁场配置的PWNe是罕见的，特别是对于发展中的系统。我们提出了一个射电偏振研究的“蜗牛”PWN内的超新星遗迹G327.1-1.1使用澳大利亚望远镜紧凑阵列。这个PWN被认为是最近被超新星（SN）反向冲击压碎的。射电形态由一个圆形主体和一个指状突起组成。我们检测到一个强大的线性极化信号的发射，这反映了一个高度有序的磁场在PWN和与混乱的磁场通常预期从流体动力学模拟的湍流环境相比。这可能意味着特征湍流尺度大于无线电波束的大小。我们建立了一个玩具模型来探索这种可能性，并发现一个模拟的PWN，其湍流尺度约为星云半径的八分之一到六分之一，脉冲星风填充因子为50- 75%，提供了与观测结果的最佳匹配。这意味着在这个系统中SN喷出物和脉冲星风物质之间的大量混合。
英文摘要：
Pulsar wind nebulae (PWNe) are suggested to be acceleration sites of cosmic rays in the Galaxy. While the magnetic field plays an important role in the acceleration process, previous observations of magnetic field configurations of PWNe are rare, particularly for evolved systems. We present a radio polarization study of the "Snail" PWN inside the supernova remnant G327.1-1.1 using the Australia Telescope Compact Array. This PWN is believed to have been recently crushed by the supernova (SN) reverse shock. The radio morphology is composed of a main circular body with a finger-like protrusion. We detected a strong linear polarization signal from the emission, which reflects a highly ordered magnetic field in the PWN and is in contrast to the turbulent environment with a tangled magnetic field generally expected from hydrodynamical simulations. This could suggest that the characteristic turbulence scale is larger than the radio beam size. We built a toy model to explore this possibility, and found that a simulated PWN with a turbulence scale of about one-eighth to one-sixth of the nebula radius and a pulsar wind filling factor of 50--75% provides the best match to observations. This implies substantial mixing between the SN ejecta and pulsar wind material in this system.
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