تقرير
Signatures of the disk-jet coupling in the Broad-line Radio Quasar 4C+74.26
| العنوان: | Signatures of the disk-jet coupling in the Broad-line Radio Quasar 4C+74.26 |
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| المؤلفون: | Bhatta, G., Stawarz, L., Markowitz, A., Balasubramaniam, K., Zola, S., Zdziarski, A. A., Jamrozy, M., Ostrowski, M., Kuzmicz, A., Ogloza, W., Drozdz, M., Siwak, M., Koziel-Wierzbowska, D., Debski, B., Kundera, T., Stachowski, G., Machalski, J., Paliya, V. S., Caton, D. B. |
| سنة النشر: | 2018 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena |
| الوصف: | Here we explore the disk-jet connection in the broad-line radio quasar 4C+74.26, utilizing the results of the multiwavelength monitoring of the source. The target is unique in that its radiative output at radio wavelengths is dominated by a moderately-beamed nuclear jet, at optical frequencies by the accretion disk, and in the hard X-ray range by the disk corona. Our analysis reveals a correlation (local and global significance of 96\% and 98\%, respectively) between the optical and radio bands, with the disk lagging behind the jet by $250 \pm 42$ days. We discuss the possible explanation for this, speculating that the observed disk and the jet flux changes are generated by magnetic fluctuations originating within the innermost parts of a truncated disk, and that the lag is related to a delayed radiative response of the disk when compared with the propagation timescale of magnetic perturbations along relativistic outflow. This scenario is supported by the re-analysis of the NuSTAR data, modelled in terms of a relativistic reflection from the disk illuminated by the coronal emission, which returns the inner disk radius $R_{\rm in}/R_{\rm ISCO} =35^{+40}_{-16}$. We discuss the global energetics in the system, arguing that while the accretion proceeds at the Eddington rate, with the accretion-related bolometric luminosity $L_{\rm bol} \sim 9 \times 10^{46}$ erg s$^{-1}$ $\sim 0.2 L_{\rm Edd}$, the jet total kinetic energy $L_\textrm{j} \sim 4 \times 10^{44}$ erg s$^{-1}$, inferred from the dynamical modelling of the giant radio lobes in the source, constitutes only a small fraction of the available accretion power. Comment: 9 pages and 6 figures, ApJ accepted |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.3847/1538-4357/aade9c |
| URL الوصول: | http://arxiv.org/abs/1805.06957 |
| رقم الأكسشن: | edsarx.1805.06957 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.3847/1538-4357/aade9c |
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