Tracking the energetics of the non-thermal disc-corona-jet in the very high state GX 339 - 4
Tracking the energetics of the non-thermal disc-corona-jet in the very high state GX 339 - 4
复制标题
跟踪非热盘电晕喷射器在极高状态下的能量 GX 339 - 4
DOI：
10.1093/mnras/stw585
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发表时间：
2016
影响因子：
4.8
通讯作者：
Chris Done
中科院分区：
文献类型：
--
作者：
Aya Kubota;Chris Done
黑洞双星中戏剧性的硬-软光谱转变很重要，因为它与喷流的坍塌和最强的低频准周期振荡(QPO)有关。这些跃迁光谱(中态和高态：VHS)是复杂的，具有柔和但明显的非热压实化，它顺利地合并到圆盘发射中。在这里，我们发展了一个物理模型，它可以适应所有这些特征，外标准盘，它可以过渡到能量耦合的盘-日冕区，并进一步过渡到热的内部流动，如果需要的话，可以是辐射低效的。代码明确使用完全相对论发射率(Novikov-Thorne)，所有康普顿化都是用混合(热和非热)电子分布计算的。我们将其与GX339和−-4的VHS谱进行了拟合。我们表明，由混合电子分布产生的复杂的连续谱曲率足以消除使用更简单的康普顿化模型的反射对黑洞自旋的强烈约束。更根本的是，我们证明了VHS不能符合相同的Novikov-Thorne发射率，该发射率可以适应圆盘主导的光谱，但要求内部流动在辐射上有些低效。这与吸积动力喷气式飞机一致，但同时的无线电数据显示，在我们的数据显示时，喷气式飞机已经坍塌。相反，正如Lense-Thirring QPO模型所预测的那样，它可能指向比最里面稳定的圆形轨道更大的半径处的内部流动截断。
The dramatic hard–soft spectral transition in black hole binaries is important as it is associated with the collapse of the jet and with the strongest low-frequency quasi-periodic oscillations (QPOs). These transition spectra (intermediate and very high state: VHS) are complex, with soft but distinctly non-thermal Comptonization which merges smoothly into the disc emission. Here we develop a physical model for the accretion flow which can accommodate all these features, with an outer standard disc, which can make a transition to an energetically coupled disc–corona region, and make a further transition to a hot inner flow which can be radiatively inefficient if required. The code explicitly uses fully relativistic emissivity (Novikov–Thorne), and all Comptonization is calculated with a hybrid (thermal and non-thermal) electron distribution. We fit this to a VHS spectrum from GX 339 − 4. We show that the complex continuum curvature produced by a hybrid electron distribution is enough to remove the strong constraint on black hole spin derived from reflection using simpler Comptonization models. More fundamentally, we show that the VHS cannot be fit with the same Novikov–Thorne emissivity which can fit the disc-dominated spectrum but instead requires that the inner flow is somewhat radiatively inefficient. This is consistent with an accretion powered jet, but simultaneous radio data show that the jet has already collapsed at the time of our data. Instead, it could point to truncation of the inner flow at radii larger than the innermost stable circular orbit, as predicted by the Lense–Thirring QPO models.