发表机构
Western Sydney University; Gifu University; Dominion Radio Astrophysical Observatory, Herzberg Astronomy & Astrophysics, National Research Council Canada; Center for Space Research and Utilization Promotion (c-SRUP), Gifu University; Department of Astronomy and Space, College of Science, University of Baghdad; Department of Astronomy, Faculty of Mathematics, University of Belgrade; Isaac Newton Institute of Chile, Yugoslavia Branch; Australia Telescope National Facility, CSIRO, Space and Astronomy; Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia（西悉尼大学; 岐阜大学; 加拿大国家研究委员会赫茨伯格天文学与天体物理学部 Dominion 射电天文台; 岐阜大学空间研究与利用促进中心（c-SRUP）; 巴格达大学理学院天文学与空间系; 贝尔格莱德大学数学学院天文学系; 智利艾萨克·牛顿研究所南斯拉夫分部; CSIRO太空与天文澳大利亚望远镜国家设施; 塞尔维亚贝尔格莱德Volgina路7号天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用ATCA与MeerKAT观测，揭示大麦哲伦云超新星遗迹N 132D的射电形态与X射线发射相关，明确其磁场特性、能量参数及射电谱特征，为研究年轻超新星遗迹的粒子加速与激波演化提供新约束。
AI 中文摘要
我们利用澳大利亚望远镜紧凑型阵列（ATCA）和MeerKAT的观测结果，对大麦哲伦云的超新星遗迹N 132D开展了一项新的射电连续谱研究。该遗迹的射电形态在其中心及左侧区域，以及壳层的右侧部分，与X射线发射呈现出清晰的空间相关性，表明热等离子体与非热等离子体成分之间存在紧密联系。偏振测量显示磁场以径向为主，在2100 MHz、5500 MHz和9000 MHz频率下的平均偏振分数分别为1.2%、3.0%和4.0%。法拉第深度谱中还存在复杂结构，呈现双峰轮廓，表明存在磁化特性不同或磁场几何形态各异的区域。从ATCA数据推导得到的旋转测量平均值约为2 rad m^-2，最大值约为338 rad m^-2。我们估算出的常划分磁场约为90 μG，最小能量为3×10^50 erg，该能量在电子能量密度与磁场能量密度之间保持常划分。积分射电谱遵循幂律分布，谱指数为-0.74±0.01。这些结果为N 132D的磁场结构和能量特性提供了新的约束，并有助于理解年轻超新星遗迹中的粒子加速与激波演化。
英文摘要
We present a new radio continuum study of the Large Magellanic Cloud supernova remnant N 132D using observations from the Australia Telescope Compact Array (ATCA) and MeerKAT. The radio morphology shows a clear spatial correlation with the X-ray emission in the central and left regions of the remnant, as well as in the right portion of the shell, indicating a close connection between the thermal and non-thermal plasma components. Polarisation measurements reveal predominantly radial magnetic fields, with mean fractional polarisations of 1.2 per cent, 3.0 per cent, and 4.0 per cent at 2100, 5500, and 9000 MHz, respectively. There is also a complex structure in the Faraday Depth spectrum, showing a double-peaked profile that indicates regions with differing magnetisation properties or varying magnetic field geometry. The rotation measure derived from ATCA data has an average value of ~2 rad m^-2, with a maximum of ~338 rad m^-2. We estimate a constant partition magnetic field of ~90 microG and a minimum energy of 3 x 10^50 erg, which is in a constant partition between the energy density of electrons and the energy density of the magnetic field. The integrated radio spectrum follows a power law with a spectral index of -0.74 +- 0.01. These results provide new constraints on the magnetic field structure and energetic properties of N 132D and offer insight into particle acceleration and shock evolution in young supernova remnants.
CommentsPublished in the Open Journal of Astrophysics
