论文标题
是什么从GRO J1655-40中的黑洞积聚盘为风提供动力？
What powers the wind from the black hole accretion disc in GRO J1655-40?
论文作者
论文摘要
黑洞积聚盘可以产生强大的流出血浆（圆盘风），被视为恒星和超级质量系统中的蓝移吸收线。类星体中的这些风在控制宇宙时间的星系形成中起着至关重要的作用，但是就它们如何物理发射尚无共识。对恒星质量黑洞GRO J1655-40的单一独特观察被用来争辩说，磁性驱动是二进制和类星体中唯一可行的机制，也是动机的统一磁风模型。 X射线加热（热辐射风）被排除在低风密度的低风密度中，从Fe XXII的亚稳态水平的吸收线估计，排除了低风密度。在这里，我们使用光电离世代码重新分析这些数据，该代码包括辐射激发的级联反应以及填充亚稳态水平的碰撞。级联反应将推断的风密度降低不仅仅是一个数量级。派生的色谱柱也是光学厚的，因此源本质上比观察到的更发光。我们表明，根据辐射流体动力学模拟计算出的热辐射风模型与数据非常匹配。我们重新审视先前的磁性风溶液，并表明这也是光学厚的，导致较大的源亮度。但是，与热辐射风不同，它难以在所需的密度下重现整个离子种群。这些结果消除了这些数据中磁风的要求，并消除了推断到类星体流出的自相似统一磁性风模型的基础
Black hole accretion discs can produce powerful outflowing plasma (disc winds), seen as blue-shifted absorption lines in stellar and supermassive systems. These winds in Quasars have an essential role in controlling galaxy formation across cosmic time, but there is no consensus on how these are physically launched. A single unique observation of a stellar-mass black hole GRO J1655-40 was used to argue that magnetic driving was the only viable mechanism and motivated unified models of magnetic winds in both binaries and Quasars. The alternative, X-ray heating (thermal-radiative wind), was ruled out for the low observed luminosity by the high wind density estimated from an absorption line of a metastable level of Fe xxii. Here we reanalyse these data using a photoionisation code that includes cascades from radiative excitation as well as collisions in populating the metastable level. The cascade reduces the inferred wind density by more than an order of magnitude. The derived column is also optically thick, so the source is intrinsically more luminous than observed. We show that a thermal-radiative wind model calculated from a radiation hydrodynamic simulation matches well with the data. We revisit the previous magnetic wind solution and show that this is also optically thick, leading to a larger source luminosity. However, unlike the thermal-radiative wind, it struggles to reproduce the overall ion population at the required density. These results remove the requirement for a magnetic wind in these data and remove the basis of the self-similar unified magnetic wind models extrapolated to Quasar outflows
