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色球网络上的物质运动分析及其加速机制的讨论
路立
Subtype硕士
Thesis Advisor丁有济
1986-07
Degree Grantor中国科学院云南天文台
Place of Conferral昆明
Abstract本文通过对太阳色球宁静区的视向小速度场的二维分布及其对应区域的Hα精细结构和光球纵向磁场的二维分布的统计分析和细节对比得出下列主要结果:1)肯定了色球Hα网络与光球磁场网络的位置统计有关性。2)宁静区磁场网络多为单极性磁场,因而网络上的磁流管一般不与其附近的磁流管组成回路。3)发现有从网络两侧超米粒元胞对应的空间上流向网络的单向水平物质流动的存在。并且这种水平流动在有较大上升运动景象的网络附近较为显著。4)色球网络上大的速度区不总是对应着很强的光球磁场分布,有许多林的上升物质流动与较弱的光球磁场分布相对应。5)亮日芒以上升为主,而暗日芒上升和下落兼而有之。6)就孤立磁流管而言,上升运动站优势。而就整个网络而言,下落运动占势。我们在观测结果和前人工作的启示下,对Roberts[1]的共振加速模型作了一些修改,得出了一个由周期性水平运动的物质流不断地挤压色球网络中的磁流管,在一定条件下,与管中传播的磁流体力学波发生共振从而加速其中的物质运动的二维线性共振加速机制的理论设想,用以解释日园而上日芒的加速,使之能与日冕中的针状体相对应。我们对这个加速机制作了详细的分析和计算并得到了令人满意的结果。我们还利用二维等离子体柱的线性小扰动的色散关系简单的讲座了磁流管在共振条件下的不稳定性。
Other AbstractBy statistical analyzing and contracting the two dimensional line-of-sight velocity fields which measured in Hα line, Hα fine structure and photospheric magnetic fields distributed in the same areas of quiet solar disk, we obtain the following most interesting results: (1) The correlation between chromospheric Hα absorption network and photospheric magnetic fieids (i.e. supergranulation boundary regions) is confirmed. (2) Most of magnetic network of quiet solar disk are mono-polarity, so that the nearby magnetic flux tubes in the network generally not form loops. (3) There are horizontal motions toward the network in chromosphere. And those motions are even evidenter in the vicinity of the network which is /found to exist upward motion. (4) The higher velocity regions in chromospheric network are not always corresponding to the stronger magnetic fields areas in photosphere. Some of them, in particular for upward motions, are corresponding to weaker magnetic fields areas in photosphere. (5) Most of bright mottles have upward motion features. But dark mottles have both upward and downward motion features almost in the same. (6) For individual flux tubes in the network, they are mainly upward motions. But for whole network, downward motion is its statistcal feature. Based on our results and previous workes in this field, we propose an idea that some spicules are results of a resonant buffeting of sides of mottles in the chromospheric network by periodic horizontal motions. For a critical wavespeed, the mottle drew energe from horizontal buffeting motions in maxism efficiency to accelerate its motion. We illustrate this effect in linear model by considering a two dimensional flux tube, i.e. mottle, embedded in an uniform compressible atmosphere. The instablity of the structure of the flux tube is discussed briefly from the dispersion relation which is drived from linera turbulent plasma equations of inside and outside of the flux tube.
Subject Area天文学
Pages57
Language中文
Document Type学位论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6572
Collection太阳物理研究组
Recommended Citation
GB/T 7714
路立. 色球网络上的物质运动分析及其加速机制的讨论[D]. 昆明. 中国科学院云南天文台,1986.
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