arXiv 1010.62012010-10astro-ph.CO

活动星系核宽线区的起源

The origin of the Broad Line Region in Active Galactic Nuclei

Bozena Czerny, Krzysztof Hryniewicz

备注：: to appear in Astronomy and Astrophysics
DOI：: 10.1051/0004-6361/201016025

摘要：

虽然宽发射线是星系核活动最可靠的标志，并且发射物质的位置可以通过混响方法很好地测量，但宽线区域形成的物理原因仍然不清楚。我们试图对它的起源进行一些限制。我们研究了宽线区下的吸积盘的性质。我们发现，在盘半径对应的位置的宽线区域，从H $β$线推断，是通用的在所有监测源，等于1000 K的有效温度。该值接近允许灰尘存在的极限值。宽线区低电离部分的可能来源是来自盘的强烈的本地尘埃风。这风变得暴露于辐射的中心区域移动时，更高的磁盘表面，随后表现得像一个失败的风，从而导致流入和流出的局部混合。这可以提供对湍流的物理解释，所述湍流既需要平滑线轮廓又需要提供额外的机械加热。

英文摘要：

Although broad emission lines are the most reliable signature of the nuclear activity of a galaxy and the location of the emitting material is well measured by the reverberation method, the physical cause of the formation of the broad line region remains unclear. We attempt to place some constraints on its origin. We study the properties of the accretion disk underlying the broad line region. We find that the effective temperature at the disk radius corresponding to the location of the broad line region, as inferred from the H$β$ line, is universal in all monitored sources and equal to 1000 K. This value is close to the limiting value that permits for the existence of the dust. The likely origin of the low ionization part of the broad line region is the strong local dusty wind from the disk. This wind becomes exposed to the irradiation by the central regions when moving higher above the disk surface and subsequently behaves like a failed wind, thus leading to a local mixture of inflow and outflow. This may provide the physical explanation of the turbulence needed both to smooth the line profiles as well as provide additional mechanical heating.

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