Title: Magnetic Field Structure of the Large Magellanic Cloud from Faraday Rotation Measures of Diffuse Polarized Emission Show Chinese title

Title: 大麦云法拉第旋转测量的磁场结构

Abstract: We present a study of the magnetic field of the Large Magellanic Cloud (LMC), carried out using diffuse polarized synchrotron emission data at 1.4 GHz acquired at the Parkes Radio Telescope and the Australia Telescope Compact Array. The observed diffuse polarized emission is likely to originate above the LMC disk on the near side of the galaxy. Consistent negative rotation measures (RMs) derived from the diffuse emission indicate that the line-of-sight magnetic field in the LMC's near-side halo is directed coherently away from us. In combination with RMs of extragalactic sources that lie behind the galaxy, we show that the LMC's large scale magnetic field is likely to be of quadrupolar geometry, consistent with the prediction of dynamo theory. On smaller scales, we identify two brightly polarized filaments southeast of the LMC, associated with neutral hydrogen arms. The filaments' magnetic field potentially aligns with the direction towards the Small Magellanic Cloud. We suggest that tidal interactions between the Small and the Large Magellanic Clouds in the past 10^9 years is likely to have shaped the magnetic field in these filaments. Show Chinese abstract

Abstract: 我们对大麦哲伦星云（LMC）的磁场进行了研究，该研究使用了在帕克斯射电望远镜和澳大利亚射电望远镜紧凑阵列在1.4 GHz处获得的弥漫偏振同步辐射数据。 观测到的弥漫偏振辐射很可能起源于银河系近侧的LMC盘面之上。 从弥漫辐射中得出的一致负旋转量（RMs）表明，LMC近侧晕中的视线磁场方向是连贯地远离我们的。 结合位于银河系背后的河外源的RMs，我们表明LMC的大尺度磁场可能具有四极几何结构，这与发电机理论的预测一致。 在较小尺度上，我们在LMC东南方向识别出两条明亮偏振的纤维，这些纤维与中性氢臂有关。 这些纤维的磁场可能与指向小麦哲伦星云的方向对齐。 我们认为，过去10^9年内小麦哲伦星云和大麦哲伦星云之间的潮汐相互作用很可能塑造了这些纤维中的磁场。