Optical variability of Mrk 421
Optical variability of Mrk 421
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DOI：
10.1007/s10509-013-1693-x
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发表时间：
2014-02
影响因子：
1.9
通讯作者：
Xu Chen;Shaoming Hu;D. Guo;J. Du
中科院分区：
文献类型：
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作者：
Xu Chen;Shaoming Hu;D. Guo;J. Du
2009年4月至2012年5月，我们在山东大学威海天文台用1.0m望远镜观测了V波段和R波段的MRK421。还收集了B波段和V波段的可用历史数据，以构建光曲线。MERK 421的亮度在B波段为11.40~16.14，在V波段为11.38~14.56。Jurkevich方法和结构函数方法的分析表明，由于其长周期变化，可能的周期约为1.36年。这一周期可以用一个封闭的二元黑洞系统模型来解释，该模型的初级黑洞质量为1.7×108m⊙，次级黑洞质量为(0.49-2.9)×107m∼。我们展示了mrk 421的颜色变化，在其较低的状态下，当其行为较亮时，其颜色更蓝。对光谱指数变化的分析表明，仅有宿主星系的贡献不足以解释MRK421的光谱指数变化，需要一些内在的机制。
We observed Mrk 421 in V and R band using the 1.0 m telescope at Weihai Observatory of Shandong University since 2009 April to 2012 May. The available historical data in B and V band were also assembled for constructing light curves. The brightness of Mrk 421 ranges from 11.40 to 16.14 in the B band light curve, and from 11.38 to 14.56 in the V band. Analyses with the Jurkevich method and the structure function method showed a possible period of about 1.36 years for its long periodic variability. This period could be explained by a close binary black hole system (BBHS) model with a primary black hole mass of 1.70×108M⊙and a secondary ∼(0.49–2.9)×107M⊙. We showed the color variability of Mrk 421, a bluer when brighter behavior during its lower state. Analyses of spectral index variations show that only a host galaxy contribution is not sufficient to explain the spectral index variations in Mrk 421, and some intrinsic mechanism is needed.