黑子活动区流场精细结构

本文通过太阳活动区光球和色球速度场和磁场观测资料,讨论了黑子活动区附近流场的精细结构,论述了太阳大气中物质的流动呈纤维结构,以及速度场纤维与磁场,色球纤维和网络结构之间的关系。     

Comparison of Five Numerical Codes for Automated Tracing of Coronal Loops

The three-dimensional (3D) modeling of coronal loops and filaments requires algorithms that automatically trace curvilinear features in solar EUV or soft X-ray images. We compare five existing algorithms that have been developed and customized to trace curvilinear features in solar images: i) the oriented-connectivity method (OCM), which is an extension of the Strous pixel-labeling algorithm (developed by Lee, Newman, and Gary); ii) the dynamic aperture-based loop-segmentation method (developed by Lee, Newman, and Gary); iii) unbiased detection of curvilinear structures (developed by Steger, Raghupathy, and Smith); iv) the oriented-direction method (developed by Aschwanden); and v) ridge detection by automated scaling (developed by Inhester). We test the five existing numerical codes with a TRACE image that shows a bipolar active region and contains over 100 discernable loops. We evaluate the performance of the five codes by comparing the cumulative distribution of loop lengths, the median and maximum loop length, the completeness or detection efficiency, the accuracy, and flux sensitivity. These algorithms are useful for the reconstruction of the 3D geometry of coronal loops from stereoscopic observations with the STEREO spacecraft, or for quantitative comparisons of observed EUV loop geometries with (nonlinear force-free) magnetic field extrapolation models.     

Observations of Low-Latitude Coronal Plumes

Using Fe ix/x 17.1 nm observations from the Extreme-Ultraviolet Imaging Telescope (EIT) on the Solar and Heliospheric Observatory (SOHO), we have identified many coronal plumes inside low-latitude coronal holes as they transited the solar limb during the late declining phase of cycle 23. These diffuse, linear features appear to be completely analogous to the familiar polar plumes. By tracking them as they rotate from the limb onto the disk (or vice versa), we confirm that EUV plumes seen against the disk appear as faint, diffuse blobs of emission surrounding a brighter core. When the EIT images are compared with near-simultaneous magnetograms from the SOHO Michelson Doppler Imager (MDI), the low-latitude, on-disk plumes are found to overlie regions of mixed polarity, where small bipoles are in contact with unipolar flux concentrations inside the coronal hole. The birth and decay of the plumes are shown to be closely related to the emergence of ephemeral regions, their dispersal in the supergranular flow field, and the cancellation of the minority-polarity flux against the dominant-polarity network elements. In addition to the faint polar and nonpolar plumes associated with ephemeral regions, we note the existence of two topologically similar coronal structures: the giant plume-like features that occur above active regions inside coronal holes, and the even larger scale “pseudostreamers” that separate coronal holes of the same polarity. In all three cases, the basic structure consists of open field lines of a given polarity overlying a photospheric region of the opposite polarity; ongoing interchange reconnection at the X-point separating the open field domains from the underlying double-arcade system appears to result in the steady evaporation of material from the closed into the open region.     

Structures in the phase space of a four dimensional symplectic map

We numerically investigate the projections of non periodic orbits in a 4-dimensional (4-D) symplectic map composed of two coupled 2-dimensional (2-D) maps. We describe in detail the structures that are produced in different planes of projection and we find how the morphology of the 4-D orbits is influenced by the features of the 2-D maps as the coupling parameter increases. We give an empirical law that describes this influence.     

2.63.8GHZ太阳微波爆发中的精细结构

微波Ⅲ型爆发和微波尖峰辐射是太阳微波爆发中两个主要的精细结构,由于微波段比长波段的情况更复杂,单从形态上很难区分。１９９４ 年Ｉｓｌｉｋｅ ＆ Ｂｅｎｚ 给出１３ＧＨｚ 频带上的各类爆发分类定义,本文参考了其中关于微波Ⅲ型爆发和微波尖峰辐射的分类,分析北京天文台２ ．６３ ．８ＧＨｚ 频带上观测到的微波尖峰辐射的精细结构,发现该定义有局限性,重新定义了本波段上的微波Ⅲ型爆发和微波尖峰辐射,并讨论了这种分类定义与设备时间分辨率的关系     

Tripolar vortex in plasma flow

Strongly nonlinear processes in a two-component plasma with sheared flow, in the low-frequency limit, in comparison with the ion gyro frequency Ω_i, and for perturbations propagating perpendicularly to the ambient magnetic field are studied. In the linear domain such a system is prone to the development of instability of the Kelvin–Helmholtz type. In the nonlinear regime this instability can saturate into stationary travelling solutions of the form of vortex chains and tripolar vortices, which are found in this paper.     

毫秒级快速尖峰辐射事件的时间和频率特性

介绍了太阳22周峰年期间云南天文台米波射电频谱仪的观测结果。主要对1557个单个Spike的时间和频率分布作了统计分析，着重指出太阳快速精细结构的观测特征并定性地指出其产生机制。     

核幔成矿物质与地幔热柱多级演化成矿

研究认为金等成矿物质主要来自核-幔源区,以气态-气液混合态、含矿流体的形式,通过地幔热柱→地幔亚热柱→幔枝构造→有利构造扩容带,迁移到幔枝构造外围的韧脆性剪切带、侵入岩体的内、外接触带、各种脉岩与围岩的接触带等有利部位集聚成矿,并构成矿田→矿床→矿体(脉)的有序排列组合,表现出不同的矿床类型。因此,应侧重研究构造成矿控矿作用,以指导新一轮地质找矿和矿产资源评价。文中还举例分析了胶西北焦家断裂与三山岛断裂的交切关系及其控矿作用。     

胶西北金矿集中区亚热柱幔枝构造成矿研究

胶西北是我国最大的黄金矿集区,不仅黄金储量巨大,而且成矿时间集中（115±5)Ma。研究认为燕山运动以来,华北东部地区进入了地幔热柱演化阶段;胶西北形成了莱阳地幔亚热柱及其外围郭家店、艾山、盘石店等幔枝构造体系。深源含矿流体通过地幔热柱→地幔亚热柱→幔枝构造→有利构造扩容带,迁移到幔枝构造的脆韧性韧脆性剪切带、侵入岩体的内、外接触带、密集的构造裂隙带、各种脉岩与围岩的接触带等有利部位集聚成矿,从而构成以幔枝构造为中心的金成矿密集区。该文以郭家店幔枝构造研究为例,分析了成矿作用,归纳了成矿模式。     

基于波场垂向和水平方向外推的高陡构造偏移

常规的单程波波动方程偏移成像方法对大角度的高陡构造偏移成像存在内在的限制.根据波动方程在各个空间方向的数学特性和高陡构造反射地震波的传播特征,通过把地震波分解为垂向的上下行波、水平方向的前后行波和左右行波,提出基于波场垂向外推和水平方向外推相结合的单程波波动方程高陡构造偏移成像方法,即用波场垂向外推的单程波波动方程偏移成像方法解决中低角度平缓构造的偏移成像,用波场水平方向外推的单程波波动方程偏移成像方法解决中高角度陡倾构造的偏移成像.这种基于波场垂向和水平方向外推相结合的高陡构造偏移成像方法是常规单程波波动方程叠前深度偏移成像方法的补充和改进,它相对基于全波方程的逆时偏移具有计算效率上的优势.