太阳光球层中的大尺度水平流。IV。大尺度水平流的垂直结构
Large-scale horizontal flows in the solar photosphere. IV. On the vertical structure of large-scale horizontal flows
摘要：
在最近的论文中，我们介绍了一种用于测量流场的方法。该方法是基于超颗粒结构的跟踪。我们并不确切地知道，它的结果是否代表光球层或某些亚光球层的流场。在本文中，结合日震数据，我们能够估计的深度在太阳对流信封，检测到的大尺度流场是很好地代表了表面测量。我们得到了一个明确的答案，我们跟踪什么样的结构，在全光盘多普勒。在平静的太阳区域，超颗粒结构被跟踪，而在有磁场的区域，磁场的结构占主导地位。这一观测结果似乎是显而易见的，因为多普勒结构的性质在磁区和平静的太阳中是不同的。我们发现，我们的方法检测到的大规模流动代表的运动层中的等离子体下降到~10微米。因此，超颗粒可以被视为对象进行的基础大规模的速度场。
英文摘要：
In the recent papers, we introduced a method utilised to measure the flow field. The method is based on the tracking of supergranular structures. We did not precisely know, whether its results represent the flow field in the photosphere or in some sub-photospheric layers. In this paper, in combination with helioseismic data, we are able to estimate the depths in the solar convection envelope, where the detected large-scale flow field is well represented by the surface measurements. We got a clear answer to question what kind of structures we track in full-disc Dopplergrams. It seems that in the quiet Sun regions the supergranular structures are tracked, while in the regions with the magnetic field the structures of the magnetic field are dominant. This observation seems obvious, because the nature of Doppler structures is different in the magnetic regions and in the quiet Sun. We show that the large-scale flow detected by our method represents the motion of plasma in layers down to ~10 Mm. The supergranules may therefore be treated as the objects carried by the underlying large-scale velocity field.
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