论文标题
X射线排放射线大通SDSS J121426.52+140258.9：光学/紫外线和X射线发射之间的独立变化
X-ray emission of radio-loud quasar SDSS J121426.52+140258.9: independent variations between optical/UV and X-ray emission
论文作者
论文摘要
为了了解主动银河核（AGN）的X射线发射，我们探索了无线电 - X射线射线变化的相关性，其无线电大通Quasar（RLQ）SDSS SDSS J121426.52+140258.9（herefter J1214+1402）与Swift和Xmmm的多型exmcccmcc of Swift和Xmmmcm comp.有了历史的多波段数据，我们发现不应由光束的射流发射统治RLQ J1214+1402的X射线通量。 Swift光学/UV和X射线光曲线表明，J1214+1402在2014年4月8日之前的光通量较低，在2014年6月11日之后的高速升高，但在2007年3月9日至2014年3月9日至2014年8月4日之间没有显着X射线变化，这是由XMM-Newton observations the xmm-newton oppervation the xmm-newton of Swift swips swipt swift swift swipt的支持。有趣的是，当J1214+1402的光学通量相对较低，但最明亮的X射线通量时，快速时间之前的XMM Newton数据呈现了两个异常发射时期。光学到X射线变化的总体独立性似乎很难由磁盘 - 核心模型描述。使用X射线光谱拟合，我们发现J1214+1402中的软X射线过量仅在X射线发射处在低状态时才会出现在高光学状态下。 J1214+1402中的软X射线过量很难用电离积聚磁盘来解释，相反，它可能与温暖的电晕有关。
To understand the X-ray emission of active galactic nuclei (AGNs), we explored the optical-to-X-ray variation correlation of a radio-loud quasar (RLQ) SDSS J121426.52+140258.9 (hereafter J1214+1402) with multi-epoch observations of Swift and XMM-Newton telescopes. With the historical multi-band data, we found that the infrared to X-ray flux of RLQ J1214+1402 should not be dominated by the beamed jet emission. The Swift optical/UV and X-ray light curves showed that J1214+1402 has two optical states with low flux before 2014 April 08 and high flux after 2014 June 11, but has no significant X-ray variations during the time range between 2007 March 09 and 2014 August 04. This result was supported by the XMM-Newton observations in the overlapped time with Swift. Interestingly, the early XMM-Newton data prior to the Swift time presents two unusual emission epochs when J1214+1402 has relatively low optical fluxes but has the brightest X-ray fluxes. The overall independence of optical-to-X-ray variation seems hard to be described by the disk-corona model. With the X-ray spectral fitting, we find that the soft X-ray excess in J1214+1402 appears only during the high optical state when the X-ray emission is at low state. The soft X-ray excess in J1214+1402 is difficult to be explained by the ionized accretion disk, instead, it may be related to the warm corona.
