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首页> 外文期刊>The Astrophysical journal >STRUCTURE AND MAGNETIC FIELDS IN THE PRECESSING JET SYSTEM SS 433. I. MULTIFREQUENCY IMAGING FROM 1998
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STRUCTURE AND MAGNETIC FIELDS IN THE PRECESSING JET SYSTEM SS 433. I. MULTIFREQUENCY IMAGING FROM 1998

机译：预处理射流系统SS 433中的结构和磁场。I. 1998年以来的多频成像

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The Very Large Array has been used at five frequencies to study the structure and linear polarization of SS 433 on scales as smallas ～0.1″ approx= 500 AU. Each jet consists of a sharp, curving ridgeline at the leading edge, plus significant trailing off-jet emission, showing that they are enveloped by diffuse relativistic plasma. No kinematic model with constant jet speed fits our images on all scales, but they are consistent with variations in jet speed of around ± 10% around the optical value. Our images show continuous jets with bright components occurring simultaneously in the two jets roughly every 35 days. When corrected for projection effects and Doppler boosting, the intensities of the two jets are intrinsically very similar. Fractional linear polarization up to 20% is present along the ridgelines, while the core is essentially unpolarized. The rotation measures are consistent with a foreground screen with RM approx= + 110 rad m~(-2) plus a larger, asymmetrical contribution close to the core. The apparent magnetic fields in the jets are roughly aligned with the ridgelines in most but not all of each jet. The jet is more highly polarized between the components than in the components themselves, suggesting that the mechanism that creates them compresses a tangled part of the magnetic field into a partially ordered transverse layer. The off-jet emission is remarkably highly polarized, with m approx= 50% in places, suggesting large-scale order of the magnetic field surrounding the jets. This polarized signal may confuse the determination of magnetic field orientations in the jets themselves. However, the images are consistent with a jet magnetic field that is everywhere parallel to the helices.
机译：超大型阵列已在五个频率下用于研究SS 433的结构和线性极化，规模小至约0.1英寸（约500 AU）。每个射流在其前缘处都包含一个尖锐的弯曲山脊线，以及明显的尾随尾随射流，表明它们被弥散的相对论等离子体所包围。没有恒定射流速度的运动学模型能够在所有尺度上拟合我们的图像，但它们与射流速度在光学值附近大约±10％的变化一致。我们的图像显示连续的喷射流中，明亮的成分大约每35天在两个喷射流中同时发生。当校正投影效果和多普勒增强效果时，两个射流的强度本质上非常相似。沿脊线存在高达20％的分数线性极化，而纤芯基本上是非极化的。旋转量度与具有RM大约= + 110 rad m〜（-2）的前景屏幕以及靠近核心的较大的不对称贡献相一致。射流中的视在磁场与大多数但并非所有射流中的山脊线大致对齐。射流在组件之间的极化比在组件本身中的极化更高，这表明产生它们的机制将磁场的纠结部分压缩为部分有序的横向层。尾气发射极显着地极化，在某些地方的m约为50％，这表明围绕着气嘴的磁场具有大规模的阶次。该极化信号可能会使喷射器自身中磁场方向的确定混乱。但是，图像与到处都平行于螺旋线的喷射磁场一致。

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