Silicon Solar Cells at Low Temperature

Electrical characteristics of n-p silicon solar cells have been obtained experimentally over the temperature range of +28 to ?175° and for illumination intensities from 140 to 1.5 mW/cm2. Critical parameters and their distribution are presented for several hundred solar cells from various manufacturers. The effect of cell selection either to a minimum power output at 28° at 5 mW/cm2 or to a minimum open-circuit voltage at ?128° at 5.16 mW/cm2 upon the magnitude and distribution of the critical parameters is investigated. Considerable differences are noted, not just between cells, but also between lots from various manufacturers. Correlation analysis reveals no parameter which when measured at room temperature will predict the power output at low temperatures. This is due to a number of anomalies of the output characteristics at low temperature. These are a lack of the open voltage to continue to increase with decreasing temperature and a double break in the current-voltage characteristics. In addition, some cells show low shunt resistance which makes them have a poor performance at low intensities.     

Review of Radiation Damage to Silicon Solar Cells

This paper reviews a large number of silicon solar cell irradiation experiments performed over the last 10 years, including 1-MeV and energy spectrum electron studies, and low-(100-keV) and high-energy (up to 155-MeV) proton studies on bare and covered silicon solar cells of several types. The results of satellite flight experiments on individual solar cells are also presented, as well as data from complete solar arrays and data on the new high-efficiency solar cells. Experimental evidence indicates that the percentage of degradation is smaller in thin solar cells than in thick ones, and that cells with high resistivity (10 ?·cm) degrade less than cells with lower resistivity (1 ?·cm). It is shown that high-efficiency silicon solar cells produced at COMSAT Laboratories and pilot production groups of these cells retain most of their increased power output under irradiation. It is emphasized that all surfaces and edges of the solar cells must be completely shielded from the large flux protons in the space environment. Insufficiencies in the published data are noted in certain areas, and recommendations for additional research are presented. Finally, an extensive bibliography is included.     

Silicon Solar Cell Performance at High Intensities

The theoretical and experimental work performed since 1960 in the area of high-intensity and high-temperature operation of silicon and gallium arsenide photovoltaic devices is reviewed. Test results for conventional 5-grid silicon cells, for specially designed 13-grid silicon cells, and for a GaAs cell are presented parametrically for the illumination intensity range from 0.07 to 2.8 W/cm2 and the temperature range from 30 to 1 50°C. The data cover the 3 points on the currentvoltage characteristic required to reconstruct the full characteristic in the power-generating quadrant. The 13-grid silicon cells showed much better performance than the GaAs cell.     

航空发动机高、低温起动及高原起动试验技术探讨

根据GJB241对航空发动机高、低温起动及高原起动试验的要求,分析了高、低温及高原环境条件对航空发动机起动性能的影响机理;阐述了利用自然环境条件、低温起动室及高空模拟试验台进行航空发动机高、低温起动及高原起动试验的优、缺点;结合国产斯贝MK202发动机分别在英国R.R.公司低温起动室和高空模拟试车台进行的低温起动试验方法和俄罗斯中央航空发动机研究院(CIAM)高空台的发动机高、低温起动及高原起动试验的方法,提出了符合我国国情的航空发动机高、低温起动及高原起动试验的实施途径。      

Ion Temperatures as Observed in a Solar Coronal Hole

From the widths of the extreme ultraviolet (EUV) lines measured by the SUMER instrument on SOHO, it was found previously (Tu et al. 1998) that the average temperature of Ne⁺⁷, at heights (relative to h₀) above the southern solar limb from 17″ to 64″, ranges between 1.3 and 5 × 10⁶ K and of Ne⁺⁶ between 1 and 4 × 10⁶ K. For mass-per-charge numbers greater than 4 the temperatures of the ions increase slightly with increasing mass-per-charge, while the thermal speed reveals no clear trend. We present a new data set with exposure times much longer than the ones in the previous study. The results obtained from line width analysis of Fe XII (1242 Å), Mg X (1249 Å), Mg VIII (772 Å) Ne VIII (770 Å), and Si VIII (1445 Å) support our previous study. In this case, the trend of increasing temperature begins at a mass-per-charge number of 3. A qualitative explanation based on ion-cyclotron-resonance heating within linear kinetic theory is suggested.     

Solar Wind Composition at Solar Maximum

Although coronal mass ejections have traditionally been thought to contribute only a minor fraction to the total solar particle flux, and although such events mainly occur in lower heliographic latitudes, the impressive spectacle of eruptions - observed with SOHO/LASCO even at times of solar minimum - indicates that an important part of the low-latitude solar corona is fed with matter and magnetic fields in a highly transient manner. Elemental and isotopic abundances determined with the new generation of particle instruments with high sensitivity and strongly enhanced time resolution indicate that, apart from FIP/FIT-fractionation, mass-dependent fractionation can also influence the replenishment of the thermal ion population of the corona. Furthermore, selective enrichment of the thermal coronal plasma with rare species such as ³He can occur. Such compositional features have until recently only been found in energetic particles from impulsive flare events. This review will concentrate on this and other aspects of the present solar maximum and conclude with some outlook on future investigations of near-terrestrial space climate (the generalized counterpart of ‘space weather’). This revised version was published online in August 2006 with corrections to the Cover Date.     

低马赫数流动中的预处理Euler方程的收敛特性

对预处理后Euler方程在低马赫数流动数值模拟中的收敛特性进行了细致研究。首先采用量级分析法研究了Weiss-Smith预处理方法对低速情形下Euler方程收敛性的影响;然后针对低速情形下预处理后的Euler方程组中各方程的收敛性,提出了一个改进的预处理矩阵。数值模拟结果表明：Weiss-Smith预处理方法可以很好地改善Euler方程在低速流动时的收敛特性,并且改进后的预处理矩阵在连续方程的收敛特性方面效果明显。     

Analysis of Performance Degradation in CdS Solar Cells

The effect of changes in five physically meaningful parameters on the I-V (current-voltage) curve of a CdS solar cell is calculated. Comparisons between the calculated data and performance data obtained from degraded solar cells are made. The parameter that changed to cause the degradation in each cell becomes apparent.     

带有太阳电池阵的卫星电源系统在轨测试方法

根据带有太阳帆板的地球同步卫星在轨测试需求,分析了星上电源系统的组成及技术状态;并以光照区可调节母线为例。给出了卫星电源系统在轨测试方法及相应的计算公式;最后,通过工程验证了该方法的正确性。     

Abundances,Ionization States,Temperatures, and FIP in Solar Energetic Particles

The relative abundances of chemical elements and isotopes have been our most effective tool in identifying and understanding the physical processes that control populations of energetic particles. The early surprise in solar energetic particles (SEPs) was 1000-fold enhancements in \({}^{3}\mbox{He}/{}^{4}\mbox{He}\) from resonant wave-particle interactions in the small “impulsive” SEP events that emit electron beams that produce type III radio bursts. Further studies found enhancements in Fe/O, then extreme enhancements in element abundances that increase with mass-to-charge ratio \(A/Q\), rising by a factor of 1000 from He to Au or Pb arising in magnetic reconnection regions on open field lines in solar jets. In contrast, in the largest SEP events, the “gradual” events, acceleration occurs at shock waves driven out from the Sun by fast, wide coronal mass ejections (CMEs). Averaging many events provides a measure of solar coronal abundances, but \(A/Q\)-dependent scattering during transport causes variations with time; thus if Fe scatters less than O, Fe/O is enhanced early and depleted later. To complicate matters, shock waves often reaccelerate impulsive suprathermal ions left over or trapped above active regions that have spawned many impulsive events. Direct measurements of ionization states \(Q\) show coronal temperatures of 1–2 MK for most gradual events, but impulsive events often show stripping by matter traversal after acceleration. Direct measurements of \(Q\) are difficult and often unavailable. Since both impulsive and gradual SEP events have abundance enhancements that vary as powers of \(A/Q\), we can use abundances to deduce the probable \(Q\)-values and the source plasma temperatures during acceleration, ≈3 MK for impulsive SEPs. This new technique also allows multiple spacecraft to measure temperature variations across the face of a shock wave, measurements otherwise unavailable and provides a new understanding of abundance variations in the element He. Comparing coronal abundances from SEPs and from the slow solar wind as a function of the first ionization potential (FIP) of the elements, remaining differences are for the elements C, P, and S. The theory of the fractionation of ions by Alfvén waves shows that C, P, and S are suppressed because of wave resonances during chromospheric transport on closed magnetic loops but not on open magnetic fields that supply the solar wind. Shock waves can accelerate ions from closed coronal loops that easily escape as SEPs, while the solar wind must emerge on open fields.     

Sensitivity of Low Frequency Oscillations to Updated Solar Models

A large number of acoustic frequencies have already been detected, leading to a "seismic" model of the Sun rather close to the actual standard solar models. The core however is not yet well constrained by these observations and frequencies of low degree, low frequency modes which penetrate deeply into the solar core are needed. We present here a study on the sensitivity of low degree low frequency (50 - 900 μHz) modes to the structure of the solar interior, in order to help their detection and identification in the low frequency spectrum observed by SoHO experiments like VIRGO and GOLF. The frequencies of p and g modes have been computed for a set of solar models with updated physics (Morel et al., 1997). We analyze their sensitivity to solar parameters like age and metallicity, and to various physical processes, like convective core overshoot and mass loss during the beginning of solar evolution. This revised version was published online in June 2006 with corrections to the Cover Date.     

ATS-6 Parabolic Antenna for Mounting Solar Cells

Calculations are made to obtain the raw electrical power that can be generated by using an ATS-6 type deployable parabolic dish as a surface for mounting solar cells without seriously interfering with its normal function as an antenna. A minimum of a few hundred watts to a maximum of a few kilowatts are generated during the apparent course of the Sun around the spacecraft. Academically, it seems that deployable solar cell panels along with their booms can be avoided.     

低温环境下RP-3航空煤油雾化特性试验研究

为了获取低温对RP-3航空煤油雾化特性的影响,在综合试验台上完成了供油压力为300～700 kPa、燃油温度为25、-15、 -35 ℃的某喷嘴雾化特性试验。使用高速摄像机拍摄雾化图像,利用Matlab/GUI图像处理功能编制的程序提取雾化锥角边缘,并 获得雾化锥角,使用相位多普勒粒子分析仪测得距喷口7 mm和17 mm处截面的雾化粒度和油滴平均速度。结果表明：在压力一 定、温度降低时,雾化锥角变小,油滴雾化粒度增大,油滴平均速度升高,在同测量截面上的油滴平均速度变化量减小;随着压力升 高,-35 ℃和25 ℃的雾化锥角相差不超过1°,-35 ℃的油滴雾化粒度增幅减小到8.36%。     

高低温环境下金属橡胶材料疲劳特性试验研究

以高低温等太空极端环境中的减振需求为背景，对设计制作的固支圆盘型金属橡胶试件进行了高低温环境疲劳特性试验研究，并根据刚度衰退特性提出了金属橡胶构件的疲劳失效判据。研究结果表明：金属橡胶材料的疲劳破坏形式主要是金属丝的断裂破碎和磨损，宏观上表现为试件动态刚度的不断衰减，且在相同振幅下，金属橡胶试件的刚度衰减速度随环境温度的降低而加快，随温度的升高而减缓。在整个疲劳试验过程中，试件损耗因子变化幅度较小，阻尼性能相对比较稳定。     

SiCp/Al复合材料在太阳电池阵展开机构上的应用

介绍了SiCp/Al复合材料的机械性能、热力学性能、加工性能，以及在太阳电池阵展开机构中的应用情况。分析认为采用SiCp/Al复合材料，充分发挥了其高比模量、高比强度和良好的耐磨性能，其管材、型材已达到了应用阶段。     

Novel DSC-IPM for Compact Converters at Elevated Temperatures

A novel two-side cooling for integrated power modules (IPMs) for improved compactness and capability for elevated temperature operations is presented. This approach applies and improves off-the-shelf products of IPM without significantly changing original packaging and fabrication process. It can reduce a device's p-n junction-temperature rise by 20% at an equivalent load, thus increasing operating ambient temperatures, which is desirable for aircraft applications. The size and volume associated with a conventional cooling mechanism can be reduced, achieving improved compactness and power density.     

Characteristics of Disorder and Defect in Hydrogenated Amorphous Silicon Nitride Thin Films Containing Silicon Nanograins

The hydrogenated amorphous silicon nitride （SiNx） thin films embedded with nano-structural silicon were prepared and the micro- structures at the interface of silicon nano-grains/SiNx were identified by the optical absorption and Raman scattering measurements. Characterized by the exponential tail of optical absorption and the band-width of the Raman scattering TO mode, the disorder in the interface region increases with the gas flow ratio increasing. Besides, as reflected by the sub-gap absorption coefficients, the density of interface defect states decreases, which can be attributed to the structural mismatch in the interface region and also the changes of hydrogen content in the deposited films. Additional annealing treatment results in a significant increase of defects and degree of disorder, for which the hydrogen out-diffusion in the annealing process would be responsible.     

铝合金在低温下的力学性能

阐述了铝合金在低温下的力学性能随温度的变化规律：在低温下拉伸性能提高、韧性改善、疲劳强度增加,且介质不同铝合金表现出不同的力学性能。并分析了这些力学性能变化规律的机理,同时对在极低温下某些铝合金锯齿变形的现象、特征、形成机理以及对力学性能的影响作了分析说明。     

不同温度下IC10合金的本构关系

 利用材料试验机（MTS809）测得IC10合金在很宽的温度范围（25~800 ℃）和不同应变率（10^-5~10^-2s^-1）内的应力 应变曲线。试验结果表明：室温下IC10合金的流变行为对应变率不太敏感;相同应变率（10^-4s^-1）下,流变行为对温度较敏感;在不同应变率、25~800 ℃温度范围内,IC10合金的屈服应力变化很小。基于试验数据,修正并拟合了Johnson-Cook方程,并利用该方程对不同温度和不同应变率下IC10合金的流变应力进行预测。与试验数据对比表明,修正后的Johnson-Cook方程能较好地描述IC10合金在不同的温度和应变率条件下的流变行为。     

Sources of Solar Wind at Solar Minimum: Constraints from Composition Data

In this discussion of observational constraints on the source regions and acceleration processes of solar wind, we will focus on the ionic composition of the solar wind and the distribution of charge states of heavy elements such as oxygen and iron. We first focus on the now well-known bi-modal nature of solar wind, which dominates the heliosphere at solar minimum: Compositionally cool solar wind from polar coronal holes over-expands, filling a much larger solid angle than the coronal holes on the Sun. We use a series of remote and in-situ characteristics to derive a global geometric expansion factor of?～5. Slower, streamer-associated wind is located near the heliospheric current sheet with a width of 10–20°, but in a well-defined band with a geometrically small transition width. We then compute charge states under the assumption of thermal electron distributions and temperature, velocity, and density profiles predicted by a recent solar wind model, and conclude that the solar wind originates from a hot source at around 1 million?K, characteristic of the closed corona.