冕流

背景磁场由含3个闭合双极场的冕流和带赤道中性电流片的开放场构成，磁绳位于中心双极场的下方，其特性由环向磁通和轴向磁通表征。

The background field consists of a coronal streamer containing three closed bipolar fields and an open magnetic field with an equatorial current sheet .

两冕流间CME事件数值模拟的改进

Improvement on the CME numerical simulation of CME between two streamers

CME和冕流结构相互作用机制的数值模拟研究

A numerical simulation study on the mechanism of interaction between CME and helmet streamer

在子午面内，研究具有嵌套闭磁场结构冕流背景对触发日冕物质抛射（CME）特征的影响。

The influence of a streamer background with nested close magnetic structures on the properties of CME initiated from its bottom is investigated in a solar meridian plane .

在两个冕流间采用具有同心圆磁场位形的触发模型触发CME事件，研究CME的日冕传播特征。

Then the CME triggering model with concentrically circular closed magnetic field structure is taken to trigger CME between two streamers for research about CME propagating features near corona .

模拟结果表明，CME被约束在两冕流间传播，CME闭磁场位形和磁云横截面磁场位形相似，可以解释1AU处观测磁云的部分特征；

The numerical result shows that the CME event is confined by the two streamers to propagate between them and the closed CME magnetic field structure is similar to that in the section of magnetic cloud , which can explain some features of magnetic cloud observed at 1 AU .

当一个日冕物质抛射伴随冕流产生时，冕流的经向角大小若大于27°，可导致冕流尖角区顶部上升速度大于2km／s。

The rise velosity of the top of the cusp region in a coronal streamer may be more than 2km / s , if the longitude angular size is more than 27 ° associated with a CME occurence .

两冕流间的对称径向膨胀日冕物质抛射事件

Radial expansion of a symmetrical CME between two coronal streamers

两冕流间物质抛射事件的数值模拟

Numerical simulation of coronal mass ejections between two coronal streamers

冕流与日冕物质抛射的关系

The relationship between coronal streamers and CMES

冕流带偏振亮度的分布是不均匀的，不均匀度为10%－50%。

The distribution of the polarization brightness along streamer belts is inhomogeneous ; the degree of the inhomogeneity is 10 % - 50 % .

日冕的边上，甚至泻出了奇异的光彩，向外辐射，出现特大的光束，天文学家称之为冕流。

Day Mian side go up , even Xie have made curious brilliance , radiate outward , arise especially big light beam , astronomer name is " Mian flow " .

结果表明：在新的扰动磁场作用下，原冕流底部的物质将受到压缩并向上运动，形成高密度亮环结构，在环的下方出现低密度暗腔；

The numerical results showed that the material contained originally in the streamer is compressed and lifted upward by the new erupting magnetic field , forming a high density bright loop , and a dark resign with low density come out below it .

本文取带赤道电流片的冕流结构作为背景，用冕流底部的磁通量喷发作为驱动机制，对日冕物质喷射触发的慢激波进行数值模拟。

This paper presents a numerical simulation of the slow shock triggered by a coronal mass ejection , taking a coronal streamer with an equatorial electric current sheet as the background as well as a magnetic flux eruption at the base of the coronal streamer as the driving mechanism .