An MHD study of SN 1006 and determination of the ambient magnetic field direction
An MHD study of SN 1006 and determination of the ambient magnetic field direction
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DOI：
10.1111/j.1365-2966.2010.17125.x
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发表时间：
2010-06
影响因子：
4.8
通讯作者：
E. Schneiter;P. Vel'azquez;E. Reynoso;F. Colle
中科院分区：
文献类型：
--
作者：
E. Schneiter;P. Vel'azquez;E. Reynoso;F. Colle
在这项工作中，我们采用磁流体动力学（MHD）的数值代码，以再现观察到的SN 1006在无线电同步辐射和热X射线发射的形态。我们引入一个密度不连续性，在一个平面云的形式平行于银河平面，为了解释观察到的光学波长和热X射线的NW灯丝。我们将我们的模型与观察结果进行比较。我们还进行了一项测试，将超新星遗迹的无线电发射明亮的边缘与中心区域进行对比，为我们的结果提供额外的支持。我们的主要结论是，环境磁场的最可能方向平均垂直于银河平面。
In this work, we employ a magnetohydrodynamic (MHD) numerical code to reproduce the morphology observed for SN 1006 in radio synchrotron and thermal X-ray emission. We introduce a density discontinuity, in the form of a flat cloud parallel to the Galactic plane, in order to explain the NW filament observed in optical wavelengths and in thermal X-rays. We compare our models with observations. We also perform a test that contrasts the radio emitting bright limbs of the supernova remnant against the central region, finding additional support to our results. Our main conclusion is that the most probable direction of the ambient magnetic field is on average perpendicular to the Galactic plane.