Measuring magnetism in the Milky Way with the Square Kilometre Array-猫眼课题宝

DOI：

10.22323/1.215.0096

发表时间：

2015-01

期刊：

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其他

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作者：

M. Haverkorn;T. Akahori;E. Carretti;K. Ferrière;P. Frick;B. Gaensler;G. Heald;M. Johnston-Hollitt;D. Jones;T. Landecker;S. A. Mao;A. Noutsos;N. Oppermann;W. Reich;T. Robishaw;A. Scaife;D. Schnitzeler;R. Stepanov;Xiao-Hui Sun;Russ Taylor

银河系中的磁场存在于各种各样的大小和强度上，影响着银河系生态系统中的许多过程，如星星形成、气体动力学、喷流和超新星遗迹或脉冲星风星云的演化。观测方法是复杂和间接的，其中最常用的是一个网格的旋转措施的未解决的极化河外源，和宽带偏振的漫发射。目前对银河系磁场的研究揭示了一个具有显著湍流成分的全球螺旋磁场;对超新星遗迹和HII区域等离散天体的磁场测量的有限样本显示了各种各样的场配置;已经发表了一些对年轻恒星天体喷流磁场的探测;银河系中心的磁场结构仍在争论中。SKA将在亚秒差距到星系尺度上揭示银河系磁场的3D结构和配置，包括银河系中心的磁场结构。通过脉冲星RM探测的银河系盘磁场的全球配置将解决关于银河系平面反转的争议。星际湍流的特征可以从背景RM的网格中确定。由于SKA可能极大地增加了样本量，我们希望能够了解原恒星喷流、超新星遗迹和其他离散源中的磁场结构。银河系磁场的知识不仅对理解银河系结构的演变和相互作用至关重要，而且还有助于为大量的河外和宇宙学研究确定和消除银河系前景。用平方公里阵列推进天体物理学

Magnetic fields in the Milky Way are present on a wide variety of sizes and strengths, influencing many processes in the Galactic ecosystem such as star formation, gas dynamics, jets, and evolution of supernova remnants or pulsar wind nebulae. Observation methods are complex and indirect; the most used of these are a grid of rotation measures of unresolved polarized extragalactic sources, and broadband polarimetry of diffuse emission. Current studies of magnetic fields in the Milky Way reveal a global spiral magnetic field with a significant turbulent component; the limited sample of magnetic field measurements in discrete objects such as supernova remnants and HII regions shows a wide variety in field configurations; a few detections of magnetic fields in Young Stellar Object jets have been published; and the magnetic field structure in the Galactic Center is still under debate. The SKA will unravel the 3D structure and configurations of magnetic fields in the Milky Way on sub-parsec to galaxy scales, including field structure in the Galactic Center. The global configuration of the Milky Way disk magnetic field, probed through pulsar RMs, will resolve controversy about reversals in the Galactic plane. Characteristics of interstellar turbulence can be determined from the grid of background RMs. We expect to learn to understand magnetic field structures in protostellar jets, supernova remnants, and other discrete sources, due to the vast increase in sample sizes possible with the SKA. This knowledge of magnetic fields in the Milky Way will not only be crucial in understanding of the evolution and interaction of Galactic structures, but will also help to define and remove Galactic foregrounds for a multitude of extragalactic and cosmological studies. Advancing Astrophysics with the Square Kilometre Array

Measuring magnetism in the Milky Way with the Square Kilometre Array

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