高温相变单元管蓄热过程数值模拟

对以高温共晶盐 Li F-Ca F2 为相变材料 (PCM)和以干空气为工质的相变蓄热系统 ,采用焓方法建立了以控制体单元为对象的单管相变蓄热模型。在模拟空间站太阳能吸热 /储热器轨道运行参数下进行了数值计算。计算结果与地面模拟试验数据进行了比较 ,吻合良好。     

Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.     

Solar Irradiance Variability Since 1978

Since November 1978 a set of total solar irradiance (TSI) measurements from space is available, yielding a time series of more than 25 years. Presently, there are three TSI composites available, called PMOD, ACRIM and IRMB, which are all constructed from the same original data, but use different procedures to correct for sensitivity changes. The PMOD composite is the only one which also corrects the early HF data for degradation. The results from the detailed analysis of the VIRGO radiometry allow a good understanding of the effects influencing the long-term behaviour of classical radiometers in space. Thus, a re-analysis of the behaviour of HF/NIMBUS-7 and ACRIM-I/SMM was indicated. For the former the situation is complicated by the fact that there are no in-flight means to determine changes due to exposure to solar radiation by comparison with a less exposed radiometer on the same spacecraft. The geometry and optical property of the cavity of HF is, however, very similar to the PMO6-type radiometers, so the behaviour of the PMO6V radiometers on VIRGO can be used as a model. ACRIM-I had to be revised mainly due to a henceforth undetected early increase and a more detailed analysis of its degradation. The results are not only important for solar radiometry from space, but they also provide a more reliable TSI during cycle 21. The differences between the revised PMOD composite and the ACRIM and IRMB are discussed by comparison with a TSI reconstruction from Kitt-Peak magnetograms. As the PMOD composite is the only one which has reliable data for cycle 21, the behaviour of the three solar cycles can now be compared and the similarities and differences discussed.     

What do Cosmogenic Isotopes Tell us About Past Solar Forcing of Climate?

In paleoclimate studies, cosmogenic isotopes are frequently used as proxy indicators of past variations in solar irradiance on centennial and millennial timescales. These isotopes are spallation products of galactic cosmic rays (GCRs) impacting Earth's atmosphere, which are deposited and stored in terrestrial reservoirs such as ice sheets, ocean sediments and tree trunks. On timescales shorter than the variations in the geomagnetic field, they are modulated by the heliosphere and thus they are, strictly speaking, an index of heliospheric variability rather than one of solar variability. Strong evidence of climate variations associated with the production (as opposed to the deposition) of these isotopes is emerging. This raises a vital question: do cosmic rays have a direct influence on climate or are they a good proxy indicator for another factor that does (such as the total or spectral solar irradiance)? The former possibility raises further questions about the possible growth of air ions generated by cosmic rays into cloud condensation nuclei and/or the modulation of the global thunderstorm electric circuit. The latter possibility requires new understanding about the required relationship between the heliospheric magnetic fields that scatter cosmic rays and the photospheric magnetic fields which modulate solar irradiance.     

Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

High-Frequency Radio Signatures of Solar Eruptive Flares

Several examples of the radio emission of eruptive solar flares with high-frequency slowly drifting structures and type II bursts are presented. Relationships of these radio bursts with eruptive phenomena such as soft X-ray plasmoid ejection and shock formation are shown. Possible underlying physical processes are discussed in the framework of the plasmoid ejection model of eruptive solar flares. On the other hand, it is shown that these radio bursts can be considered as radio signatures of eruptive solar flares and thus used for the prediction of heliospheric effects. This revised version was published online in August 2006 with corrections to the Cover Date.     

空间站大面积太阳翼热分析

本文在一定的假设条件下，对空间站大面积太阳翼进行了系统的热流和温度场计算。在计算中利用矢量分析和坐标变换的方法求解出了太阳直接辐射1地球红外辐射和地球反照的辐射角系数，再根据传热学理论建立了瞬态热平衡方程，应用有限单元法对热平衡方程进行了求解。本文通过计算给出了各项热流的大小及在总热流中所占的比例和太阳民办的瞬态温度场分布，对空间站大面积太阳翼设计及热控制具有一定的参考价值。     

关于阵列式雷达目标模拟器的理论分析

本文权述了阵列式雷达目标模拟器的基本原理。根据模拟目标与实际目标在接收处的反射场及视在中心均应相同的关系导出了三元阵三个阵元的调制信号,并指出这种射频目标仿真既适用于单站情况,也适用于双站情况。     

ESPRIT算法在单快拍阵列信号中的应用

ESPRIT算法利用旋转不变技术估计信号参数,是近年来提出的阵列信号处理理论的一个新领域,它具有高分辨率、高精度、不需空间搜索等优点。单快拍总被当作相干信号处理,本文采用了Teoplitz结构协方差矩阵估计,起了空间平滑作用,所以可以估计相于信号源的波达方向(DOA),与标准空间平滑协方差矩阵估计相比较,Teoplitz协方差阵估计在总体上提高了信噪比,并且不牺牲阵列孔径。 计算机模拟结果表明,基于Teoplitz结构协方差矩阵的TLS-ESPRIT算法在20dB信噪比下,可以分辨出相隔0.2瑞利波束宽度的空间信号。     

基于数字滤波的B-样条插值法在图像旋转中的应用

提出一种基于无限脉冲响应和有限脉冲响应数字滤波技术的快速 B-样条插值法 ,并将其应用于实时图像旋转处理中。为了优化旋转后的图像质量 ,本文采用 3次 B-样条对图像旋转后的像素点灰度值进行插值运算。另外 ,通过对传统图像旋转矩阵的分解 ,将图像在二维空间中的旋转运算分解成为三步在一维空间内平移运算 ,使插值运算在一维空间中完成 ,从而简化了图像旋转数据处理中的插值运算。最后 ,还提出了一种以硬件方法完成高阶图像插值运算实现图像旋转的新方法 ,并针对 2 5 6灰度级 ,2 5 6× 2 5 6像素的图像 ,设计出一个以 FPGA为核心的实时、高质量的硬件图像旋转系统。