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1.
The structure and dynamics of a box in a stellar corona can be modeled employing a 3D MHD model for different levels of magnetic activity. Depending on the magnetic flux through the surface the nature of the resulting coronal structures can be quite different. We investigate a model of an active region for two sunspots surrounded by magnetic field patches comparable in magnetic flux to the sunspots. The model results in emission from the model corona being concentrated in loop structures. In Gudiksen and Nordlund (2005) the loops seen in EUV and X-ray emission outline the magnetic field, following the general paradigm. However, in our model, where the magnetic field is far from a force-free state, the loops seen in X-ray emission do not follow the magnetic field lines. This result is of interest especially for loops as found in areas where the magnetic field emerging from active regions interacts with the surrounding network.  相似文献   

2.
We study the short-term topological changes of equatorial and polar coronal hole (CH) boundaries, such as a variation of their area and disintegration, associated to reconnection with nearby (within 15° distance) quiescent prominence magnetic fields leading to eruptions and subsequent Coronal Mass Ejections (CMEs). The examples presented here correspond to the recent solar minimum years 2008 and 2009. We consider a temporal window of one day between the CH topological changes and the start and end times of prominence eruptions and onset of CMEs. To establish this association we took into account observational conditions related to the instability of prominence/filaments, the occurrence of a CME, as well as the subsequent evolution after the CME. We found an association between short-term local topological changes in CH boundaries and the formation/disappearance of bright points near them, as well as, between short-term topological changes within the whole CH and eruptions of nearby quiescent prominences followed by the appearance of one or more CMEs.  相似文献   

3.
The evolution of coronal mass ejection/shock system is investigated by numerically solving the usual set of two-dimensional single-fluid polytropic magnetohydrodynamic equations from 1 Rs to 1 AU in the meridian plane. The simulation result reveals that the coronal mass ejection/shock system formed near the sun evolves into the magnetic cloud/shock system near the earth’s orbit through the following three phases: the initial formation, the dominant latitudinal expansion and the similar expansion.  相似文献   

4.
基于非均匀有理B样条的自由型面变形(NFFD)技术具有对变形对象普适性和控制点影响区域局部性的特点,广泛应用于气动外形优化。本文通过扩展控制体和合理布置外侧控制点,实现了NFFD技术在参数化曲面并改变曲面形状时,同步变形控制体内的表面网格和空间网格,并从理论上保证了控制体边界内外的网格协调。基于离散伴随方法求取梯度,分别采用拟牛顿(QN)法和序列二次规划(SQP)优化方法,通过从初始翼型NACA0012到标准翼型EH1590的反设计,研究了NFFD控制点数量和分布对设计结果的影响。在某飞翼标模单点全机升阻比优化应用中,改进控制点分布后获得了更高的升阻比,收敛速度显著提高。  相似文献   

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