论文标题
Q2237+0305 Quasar中的超级埃德丁顿积聚？
Super-Eddington accretion in the Q2237+0305 quasar?
论文作者
论文摘要
Q2237+0305 Quasar的通量变化之间的频带间时间滞后是根据Johnson-Cousins V，R和I光谱带的光曲线确定的。过滤器对R-V，I-R和I-V的时间滞后值明显高于Shakura和Sunyaev标准积聚磁盘模型所预测的值。为了解释差异，应用了Shakura和Sunyaev在1973年考虑的类星体中的超临界积聚制度的想法。他们已经证明了这种状态在积聚磁盘周围引起扩展的散射信封。信封有效地散布并重新散发出从积聚盘的辐射，从而增加了明显的磁盘大小。我们利用了Shakura和Sunyaev在超级 - 埃德丁顿积聚的分析中得出的包膜半径和温度的分析表达式，并表明我们的结果与存在这种信封的存在一致。计算了增生方案的相应参数。它们在V，r和I光谱带中提供了符合我们工作中确定的带间时间滞后的光谱带中的射频。
The interband time lags between the flux variations of the Q2237+0305 quasar have been determined from light curves in the Johnson-Cousins V, R, and I spectral bands. The values of the time lags for filter pairs R-V, I-R, and I-V are significantly higher than those predicted by the standard accretion disk model by Shakura and Sunyaev. To explain the discrepancy, the idea of a supercritical accretion regime in quasars considered in 1973 by Shakura and Sunyaev is applied. This regime has been shown by them to cause an extended scattering envelope around the accretion disk. The envelope efficiently scatters and re-emits the radiation from the accretion disk and thus increases the apparent disk size. We made use of analytical expressions for the envelope radius and temperature derived by Shakura and Sunyaev in their analysis of super-Eddington accretion and show that our results are consistent with the existence of such an envelope. The corresponding parameters of the accretion regime were calculated. They provide the radii of the envelope in the V, R, and I spectral bands consistent with the inter-band time lags determined in our work.
