漏斗壁射流和软X射线过剩的性质
Funnel wall jets and the nature of the soft X-ray excess
摘要：
在许多1型活动星系核中看到的平滑的软X射线过剩可以很好地用具有大速度色散的部分电离物质的吸收模型来描述，通常物理上解释为辐射驱动的吸积盘风。然而，国家的最先进的XSCORT代码，计算通过差分流出吸收器的光电离辐射转移，表明终极速度的顺序~ 0.9 c是必需的，以再现软X射线过剩。如此高的出流速度排除了紫外线驱动、连续辐射驱动和热驱动作为产生风的机制。磁驱动射流夹带的材料是这种高速流动的唯一合理来源，但射流和相关流出的数值模拟目前没有显示足够的材料在足够高的速度来再现软X射线过剩。如果软过量是由吸收产生的，那么似乎更有可能的是，该材料是clubelous和/或仅部分覆盖源，而不是形成连续的流出。
英文摘要：
The smooth soft X-ray excess seen in many type-1 AGN can be well described by models of absorption in partially ionized material with a large velocity dispersion, often physically interpreted as a radiatively driven accretion disk wind. However, the state-of-the-art XSCORT code, which calculates the photoionized radiative transfer through a differentially outflowing absorber, shows that terminal velocities of order ~0.9c are required in order to reproduce the soft X-ray excess. Such a high outflow velocity rules out UV-line driving, continuum radiation driving, and thermal driving as mechanisms for producing the wind. Entrainment of material by the magnetically driven jet is the only plausible origin of such a high velocity flow, but numerical simulations of jets and associated outflows do not currently show sufficient material at high enough velocities to reproduce the soft X-ray excess. If the soft excess is produced by absorption then it seems more likely that the material is clumpy and/or only partially covers the source rather than forming a continuous outflow.
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