Interactive Multi-objective Optimization Design for the Pylon Structure of an Airplane

The pylon structure of an airplane is very complex, and its high-fidelity analysis is quite time-consuming. If posterior preference optimization algorithm is used to solve this problem, the huge time consumption will be unacceptable in engineering practice due to the large amount of evaluation needed for the algorithm. So, a new interactive optimization algorithm-interactive multi-objective particle swarm optimization （IMOPSO） is presented. IMOPSO is efficient, simple and operable. The decision-maker can expediently determine the accurate preference in IMOPSO. IMOPSO is used to perform the pylon structure optimization design of an airplane, and a satisfactory design is achieved after only 12 generations of IMOPSO evolutions. Compared with original design, the maximum displacement of the satisfactory design is reduced, and the mass of the satisfactory design is decreased for 22%.     

Statistical study of radio drifting pulsation structures with associated CMEs and other observations

Solar radio burst, especially the fine structures (FSs) and the drifting pulsation structures (DPSs), may be used as an important diagnostics tool to draw the evolution map of the flare loop in the initial phase of solar flares. In this work, 52 radio events were found accompanying with DPSs. They were all observed with the Solar Radio Spectrometers (0.625–7.6 GHz) of China during 1998–2004. Combining the radio observations with LASCO-C2, Goes-8 SXR, H_α, EUV and Trace observations, we analyzed all these events and obtained some statistic conclusions: First, 88% DPSs take place at the initial phase of the radio burst, and their rich spectrum characteristics are helpful to understand the events further. Second, 83% DPSs are associated with CMEs or ejection events, and all the events are accompanied by Goes SXR flare. Third, for CMEs and DPSs, which take the first step, there is no significant predominance of either of them. The relationship between the DPSs and CMEs is still not clear in this study because of the lack of spatial resolution in the centimeter–decimeter band. However, the EIT or Trace ejection happened during the onset/end time of DPSs. They are signatures of the initial phase of CMEs. Two events will be illustrated to explain this.     

Remnants of compact binary mergers

We investigate the long-term evolution and observability of remnants originating from the merger of compact binary systems and discuss the differences to supernova remnants. Compact binary mergers expel much smaller amounts of mass at much higher velocities, as compared to supernovae, which will affect the dynamical evolution of their remnants. The ejecta of mergers consist of very neutron rich nuclei. Some of these neutron rich nuclei will produce observational signatures in form of gamma ray lines during their decay. The composition of the ejecta might even give interesting constraints about the internal structure of the neutron star. We further discuss the possibility that merger remnants appear as recently discovered ‘dark accelerators’ which are extended TeV sources which lack emission in other bands.     

Education and public outreach program for IHY – A global approach

Education and public outreach (EPO) is one of the four components of the International Heliophysical Year (IHY). It is fundamental in achieving one of IHY’s primary objectives which is to “demonstrate the beauty, relevance and significance of Space and Earth science to the world.”     

A question raised from the observation of dynamic cusp formation: When and where does particle acceleration occur?

We present observations of a C9.4 flare on 2002 June 2 in EUV (TRACE) and X-rays (RHESSI). The multiwavelength data reveal: (1) the involvement of a quadrupole magnetic configuration; (2) loop expansion and ribbon motion in the pre-impulsive phase; (3) gradual formation of a new compact loop with a long cusp at the top during the impulsive phase of the flare; (4) appearance of a large, twisted loop above the cusp expanding outward immediately after the hard X-ray peak; and (5) X-ray emission observed only from the new compact loop and the cusp. In particular, the gradual formation of an EUV cusp feature is very clear. The observations also reveal the timing of the cusp formation and particle acceleration: most of the impulsive hard X-rays (>25 keV) were emitted before the cusp was seen. This suggests that fast reconnection occurred during the restructuring of the magnetic configuration, resulting in more efficient particle acceleration, while the reconnection slowed after the cusp was completely formed and the magnetic geometry was stabilized. This observation is consistent with the observations obtained with Yohkoh/Soft X-ray Telescope (SXT) that soft X-ray cusp structures only appear after the major impulsive energy release in solar flares. These observations have important implications for the modeling of magnetic reconnection and particle acceleration.     

Abundances of Light Elements

This paper briefly reviews a few relevant features about the abundances of light elements (D, ⁴He, ⁶Li, ⁷Li, ⁹Be) in the Milky Way. It places special emphasis on metal-poor stars. Observational concerns are discussed. The use of ⁷Li and ⁶Li as cosmological probes and of ⁹Be as a chronometer for the early evolution of our Galaxy are discussed.     

浅谈高校财务预算的编制与执行

高校财务预算是财务管理的核心，一切财务活动都是对预算执行情况的反映。因此，编制科学、合理的预算，就要遵循一定的编制原则，按照一定的方法，使预算更加接近实际，切实可行。     

分布式电能计量与计费系统中通信信道特性与实现方案的研究

本文介绍了分布式电能计量与计费系统中低压电力线作为载波通信信道时的信道特性，给出了实验数据和特性曲线，并选择了通信的基本方案。     

可视化技术在分析新型蓄冷材料——笼型化合物(Clathrate)溶解过程中的应用(一)

混浊液内部的流动 ,由于微粒子之间的相互作用以及因浊度高不易进行内部观察 ,所以无论是分析还是可视化实验都相当困难 ,存在着许多未弄清的问题。通过采用折射率匹配 (Refractive IndexMatching)技术 ,使透明的微粒子与透明的溶媒的折射率近乎相同 ,做成一种透明的“混浊液” ,从而使混入其中的示踪粒子的运动轨迹能被摄像机捕捉到 ,并以微粒子的沉降和温度的干涉所引起的流动现象为焦点 ,利用图像速度测量法来处理分析所拍摄到的可视化图像 ,成功地获得了定量的混浊液内部的速度场 ,为进一步揭示混浊液内部自然对流的流动机理提供了实验依据。     

对会计主体的再认识及对主体权益论的质疑

本文对会计主体的认识进行了反思，认为会计主体是一组具有内在联系的、相互依存的契约所构成的契约集，并由此引发了对主体权益论的质疑，作者认为会计权益理论应当与公司的治理相统一，忽视了这一点，会计对契约效率的辅助功能就会严重受损。当前企业资产负债表中对权益的揭示方法确有待改进，会计等式或许应本着如下模式展开：即资产=负债+资本所有者权益+管理者权益。