论文标题
通过Insight-HXMT型CASI Quasi periodic振荡在Maxi J1535-571中电晕的演变
The evolution of the corona in MAXI J1535-571 through type-C quasi-periodic oscillations with Insight-HXMT
论文作者
论文摘要
当源处于低硬性和硬质状态时，黑洞X射线瞬变中的类型-C准周期振荡（QPO）可能会出现。最近已经使用Insight-HXMT研究了Maxi J1535-571中Type-C QPO的频谱定时演变。在这里，我们使用相对论反射模型同时拟合了时间平均的能量谱，以及当源在中间状态时，使用最近开发的时间依赖性的综合模型，使用了类型-C QPO的分数RMS和相位lag光谱。我们首次表明，时间依赖性的组合模型可以成功解释X射线数据最高100 keV。我们发现，在硬式中间状态下，Type-C QPO的频率从2.6 Hz降低到2.1 Hz，然后增加到3.3 Hz，最终增加到〜9 Hz。同时，电晕大小和反馈分数的演变（在电晕返回圆盘的光子上的光子的一部分）表明了电晕的形态的变化。与同时的无线电观察相比，该进化表明，当系统处于硬性中间状态并将其转移到软中间状态时，电晕和射流之间可能存在联系。
Type-C quasi-periodic oscillations (QPOs) in black hole X-ray transients can appear when the source is in the low-hard and hard-intermediate states. The spectral-timing evolution of the type-C QPO in MAXI J1535-571 has been recently studied with Insight-HXMT. Here we fit simultaneously the time-averaged energy spectrum, using a relativistic reflection model, and the fractional rms and phase-lag spectra of the type-C QPOs, using a recently developed time-dependent Comptonization model when the source was in the intermediate state. We show, for the first time, that the time-dependent Comptonization model can successfully explain the X-ray data up to 100 keV. We find that in the hard-intermediate state the frequency of the type-C QPO decreases from 2.6 Hz to 2.1 Hz, then increases to 3.3 Hz, and finally increases to ~ 9 Hz. Simultaneously with this, the evolution of corona size and the feedback fraction (the fraction of photons up-scattered in the corona that return to the disc) indicates the change of the morphology of the corona. Comparing with contemporaneous radio observations, this evolution suggests a possible connection between the corona and the jet when the system is in the hard-intermediate state and about to transit into the soft-intermediate state.
