太阳活动峰年和谷年期间黑子群与耀斑的统计分析

基于NOAA/SWPC公布的太阳活动数据,我们选取第24太阳活动峰年附近的12个连续月份(2011年7月至2012年6月)和第23太阳活动周谷年附近的12个连续月份(2005年7月至2006年6月),统计了这两段时间中太阳黑子群和耀斑的活动规律,并根据时间、黑子群分布纬度、寿命和磁场类型等对峰年和谷年进行了详细分析和比较,主要结论如下所述.(1)黑子群数随时间的变化在峰年和谷年均比较随机,峰年期间黑子数比谷年增多1.5倍左右.耀斑爆发与黑子群活动具有良好的相关性,但峰年期间存在某个月份耀斑数很少的现象,而谷年期间存在某个月份耀斑数集中增多的现象.(2)无论峰年还是谷年,δ类型黑子群的耀斑产率(耀斑总数与黑子群总数之比)最大,但β型黑子群产生的耀斑爆发最多.耀斑产率与磁场类型有密切关系,但与其所处太阳活动周中的阶段无关.(3)黑子群和耀斑的纬度分布的南北不对称性,以X级耀斑最为显著.峰年较谷年的耀斑数增加主要集中在C级和M级.(4)耀斑产率同黑子群寿命具有良好的相关性,但黑子群的数目同它们的寿命之间没有明显的规律.     

天然气处理厂放空火炬系统的稳定性分析

以苏里格气田第四处理厂的放空火炬系统为研究对象,对其破坏原因及机制进行研究,提出稳定性破坏的概念,把火炬管与塔架之间的相互作用简化为弹簧约束,利用能量法和有限元法分析火炬失稳破坏的临界条件。结果表明:内压降低了火炬管的稳定性,而外压增强了火炬管的稳定性。两种分析方法得到了很接近的结果,证明了该理论方法的可行性。     

银河系结构的再认识——2.外区的翘曲结构

银河系外部区域存在翘曲结构已是不争的事实,对不同类别示踪天体(如星族I 天体、分子云、星际尘埃、老年恒星等)实测结果的分析都确认了这一点。不过,关于翘曲结构的形成机制迄今尚未达成共识。     

XMM-Newton卫星观测大陵五数据分析

分析了XMM-Newton卫星对密近双星系统大陵五的观测数据,得出其光变曲线和能谱.通过对光变曲线的分析,得出探测到的X射线耀发的线形尺度和纬度.通过能谱随时间的演化得到了大陵五X射线冕的温度结构.     

模拟器视景系统中太阳及镜头光晕的绘制

为解决现有航海模拟器视景系统中对太阳及镜头光晕的模拟不完善、无法显示太阳、不能控制太阳及镜头光晕效果等问题,提出基于OpenGL和Cg绘制太阳及镜头光晕的方法.讨论光晕分布、纹理及融合等技术,并引入光晕边界的概念,实现光晕的淡入淡出.采用光线投射方法判断太阳与其他物体的遮挡关系,解决了z缓冲区方法无法判断视见体外物体的可见性问题,并利用顶点着色器技术对该方法进行优化.结果显示,该法简单,易于实现,绘制效果真实,满足航海模拟器对视景系统的实时性和逼真度要求.     

Absorption events associated with solar flares

During the upward period of solar cycle 23, the Imaging Riometer at Zhongshan, Antarctica (geomag. lat. 74.5 S) was used to study the solar proton events and the Xray solar flares which are associated with the absorption events. In our study, the relationship between the absorption intensity and X-ray flux is found in a power form which is consistent with the theoretical result. The imaging riometer absorption data at Ny-Ålesund, Svalbard reconfirm the above relationship. We also argue that only M-class flares can generate a significant daytime absorption.     

舒曼谐振的数据处理方法及其应用研究

舒曼谐振（Schumann resonance, SR）信号淹没于非常强的环境噪声数据中,影响了常规处理方法的性能。为了从观测数据中可靠地提取微弱的SR信号,先对实际的SR观测数据进行奇异值分解（singular value decomposition, SVD）滤波,再利用常规算法提取参数,分析了观测站处的闪电源分布、参数日变化规律以及一起太阳耀斑事件对应的参数变化。结果证明,经过SVD滤波后得到的估计结果能更好地反映SR参数的变化规律,极大地提高了常规方法的可靠性。     

A comparative analysis on two solar proton events

This paper presents a comparative analysis on the two Solar Proton Events (SPE), which occurred on 14 July 2000 (Bastille Day) and 28 October 2003 (28OCT03) respectively. It is found that although the peak flux of the latter seemed to be greater than that of the former based on geostationary observations, the maximum intensities of the energetic protons (>10 MeV and 30 MeV) during the Bastille Day event were all higher than those of the 28OCT03 event according to the interplanetary observations. Further analysis indicated that the quantity of the seed particles, which could be accelerated to the energies exceeding 10 and 30 MeV by the Coronal Mass Ejection (CME)-driven shock on 14 July 2000, was far larger than that of the 28OCT03 event. In the Bastille Day case, when the CME approached to the height around 14 R⊙, the CME-driven shock would reach its maximum capacity in accelerating the solar en- ergetic protons (>100 MeV). In contrast, on 28 October 2003, when CME approached to the height about 58R⊙, the CME-driven shock reached its highest potential in accelerating the solar energetic protons of the same category. At this moment, the peak flux (>100 MeV) was about 155 pfu, which was much lower than 355 pfu measured on 14 July 2000. This demonstrated that in the Bastille Day event, the quantity of the seed particles, which could be accelerated to the energy beyond 100 MeV, was significantly larger than its counterpart in the 28OCT03 case. Therefore, the peak flux of an SPE event depends not only on the interplanetary intensity of the solar energetic particles, but also on the velocity of the associated CME-driven shock, and the quantity of the seed particles as well as on the interplanetary magnetic en- vironment. This paper also reveals that the magnetic sheath associated with ICME on 28 October 2003 captured a large number of solar energetic protons, including those having energy greater than 100 MeV.