A Novel Method of Modeling Extended Emission of Compact Jets: Application to Swift J1727.8−1613

Andrzej A. Zdziarski, Callan M. Wood and Francesco Carotenuto
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Abstract

Flat radio spectra of compact jets launched by both supermassive and stellar-mass black holes (BHs) are explained by an interplay of self-absorbed synchrotron emission up to some distance along the jet and optically thin synchrotron at larger distances. Their spatial structure is usually studied using core shifts, in which the position of the peak (core) of the emission depends on the frequency. Here, we propose a novel and powerful method to fit the spatial dependence of the flux density at a given frequency of the jet and counterjet (when observed), using the theoretical spatial dependencies provided as simple analytical formulae. We apply our method to the spatial structure of the jets in the luminous hard spectral state of the BH X-ray binary Swift J1727.8−1613. It was the most resolved continuous jet from an X-ray binary ever observed. We find that the observed approaching jet is significantly intrinsically stronger than the receding one, which we attribute to an increase in the emission of both jets with time (observationally confirmed), together with the light travel effect, causing the receding jet to be observed at an earlier epoch than the approaching one. The jets are relatively slow, with a velocity of ∼(0.3–0.4)c. Our findings imply that the magnetic field strength increased with time. Additionally, the magnetic flux is significantly lower than in jets launched by “magnetically arrested disks.” Our method is general, and we propose that it be applied to jets launched by both stellar-mass and supermassive BHs.
一种新型紧凑型射流扩展发射建模方法:在Swift J1727.8−1613上的应用
超大质量黑洞和恒星质量黑洞(BHs)发射的紧凑型喷流的平坦射电光谱可以用自吸收同步加速器在喷流上一段距离内的发射和更远距离上的光学薄同步加速器的相互作用来解释。它们的空间结构通常使用地核位移来研究,其中发射峰(地核)的位置取决于频率。在这里,我们提出了一种新颖而强大的方法来拟合给定频率下射流和反射流(当观测到时)的通量密度的空间依赖性,使用提供的理论空间依赖性作为简单的解析公式。我们将我们的方法应用于黑洞x射线双星Swift J1727.8−1613的发光硬光谱状态下喷流的空间结构。这是迄今为止观测到的x射线双星中分辨率最高的连续喷流。我们发现观测到的渐近的喷流本质上明显强于渐近的喷流,我们将其归因于两种喷流的发射随时间的增加(观测证实),以及光传播效应,导致渐远的喷流在比渐近的喷流更早的时代被观测到。射流相对缓慢,速度为~ (0.3-0.4)c。我们的研究结果表明,磁场强度随着时间的推移而增加。此外,磁通量明显低于由“磁碟”发射的射流。我们的方法是通用的,我们建议它适用于由恒星质量和超大质量黑洞发射的射流。
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