Exploring the Variability of the Flat-spectrum Radio Source 1633+382. II. Physical Properties
Exploring the Variability of the Flat-spectrum Radio Source 1633+382. II. Physical Properties
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DOI：
10.3847/1538-4357/aac2e7
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发表时间：
2018-05
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通讯作者：
J. Algaba;Sang-Sung Lee;B. Rani;Dae-Won Kim;M. Kino;J. Hodgson;Guangyao Zhao;D. Byun;M. Gurwell;Sincheol Kang;Jae-Young Kim;Jeong-Sook Kim;Soon-Wook Kim;Jongho Park;S. Trippe;K. Wajima
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作者：
J. Algaba;Sang-Sung Lee;B. Rani;Dae-Won Kim;M. Kino;J. Hodgson;Guangyao Zhao;D. Byun;M. Gurwell;Sincheol Kang;Jae-Young Kim;Jeong-Sook Kim;Soon-Wook Kim;Jongho Park;S. Trippe;K. Wajima
平谱射电类星体1633+382 （4C 38.41）在2012年3月- 2015年8月期间，其射电通量密度显著增加，这与γ射线耀斑活动有关。多频同步甚长基线干涉测量（VLBI）观测作为伽马射线明亮活动星系核（iMOGABA）干涉监测计划的一部分进行，并辅以OVRO 40米望远镜、波士顿大学VLBI计划和亚毫米阵列的额外无线电监测观测。两个最大的γ射线耀斑的最大值与两个新的VLBI分量的喷射相吻合。光谱能量分布分析表明，耀斑事件发生后，周转率较高。耀斑在周转率-周转率通量密度平面上的演化过程与射流冲击模型一致，探讨了其绝热损失。导出的同步加速器自吸收磁场约为0.1 mG，在耀斑期间似乎没有显著变化，而且比估计的均分磁场弱104倍，这表明耀斑的来源可能与粒子主导的发射区有关。
The flat-spectrum radio quasar 1633+382 (4C 38.41) showed a significant increase of its radio flux density during the period 2012 March–2015 August, which correlates with γ-ray flaring activity. Multi-frequency simultaneous very long baseline interferometry (VLBI) observations were conducted as part of the interferometric monitoring of gamma-ray bright active galactic nuclei (iMOGABA) program and supplemented with additional radio monitoring observations with the OVRO 40 m telescope, the Boston University VLBI program, and the Submillimeter Array. The epochs of the maxima for the two largest γ-ray flares coincide with the ejection of two respective new VLBI components. Analysis of the spectral energy distribution indicates a higher turnover frequency after the flaring events. The evolution of the flare in the turnover frequency-turnover flux density plane probes the adiabatic losses in agreement with the shock-in-jet model. The derived synchrotron self-absorption magnetic fields, of the order of 0.1 mG, do not seem to change dramatically during the flares, and are much weaker, by a factor 104, than the estimated equipartition magnetic fields, indicating that the source of the flare may be associated with a particle-dominated emitting region.