演化核星团提供燃料的NGC 1068中心几秒差距区域的气体动力学
Gas dynamics of the central few parsec region of NGC 1068 fuelled by the evolving nuclear star cluster
摘要：
在甚大望远镜上用近红外自适应光学积分场摄谱仪SINFONI进行的高分辨率观测证明，在塞弗特星系样本的中心存在着大质量的年轻核星团。借助三维高分辨率流体动力学模拟与冥王星代码，我们遵循这样的集群的演变，专注于恒星质量损失。这导致了大尺度（数十秒差距）的气体聚集或对流流入，而湍流和非常密集的圆盘在秒差距尺度上形成。为了捕获内部区域的相关物理，我们通过粘性演化径向表面密度分布来单独处理该盘。这使我们能够将数十秒差距尺度区域（可通过SINFONI观测）与（亚）秒差距尺度区域（可通过水脉泽发射和使用射电望远镜观测）联系起来。在这项工作中，我们集中在一个参数化的湍流粘度的影响，以产生角动量和质量传递的光盘，并考虑到恒星的形成。输入参数受到附近的塞弗特2星系NGC 1068的观测的限制。在目前的年龄，其核恒星爆发的250万年，我们的模拟产量盘大小的顺序为0.8至0.9 pc，气体质量的1.0e6太阳质量和质量转移率的0.025太阳质量每年通过盘的内缘。这表明，我们的大尺度环面模型是能够近似占光盘的大小推断在中红外干涉观测和比较以及旋转盘结构的程度和质量推断水脉泽观测。还讨论了其他几个观察限制。
英文摘要：
High resolution observations with the NIR adaptive optics integral field spectrograph SINFONI at the VLT proved the existence of massive and young nuclear star clusters in the centres of a sample of Seyfert galaxies. With the help of three-dimensional high resolution hydrodynamical simulations with the Pluto code, we follow the evolution of such clusters, focusing on stellar mass loss. This leads to clumpy or filamentary inflow of gas on large scales (tens of parsec), whereas a turbulent and very dense disc builds up on the parsec scale. In order to capture the relevant physics in the inner region, we treat this disc separately by viscously evolving the radial surface density distribution. This enables us to link the tens of parsec scale region (accessible via SINFONI observations) to the (sub-)parsec scale region (observable with the MIDI instrument and via water maser emission). In this work, we concentrate on the effects of a parametrised turbulent viscosity to generate angular momentum and mass transfer in the disc and additionally take star formation into account. Input parameters are constrained by observations of the nearby Seyfert 2 galaxy NGC 1068. At the current age of its nuclear starburst of 250 Myr, our simulations yield disc sizes of the order of 0.8 to 0.9 pc, gas masses of 1.0e6 solar masses and mass transfer rates of 0.025 solar masses per year through the inner rim of the disc. This shows that our large scale torus model is able to approximately account for the disc size as inferred from interferometric observations in the mid-infrared and compares well to the extent and mass of a rotating disc structure as inferred from water maser observations. Several other observational constraints are discussed as well.
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