管道—楔形肋片式空间辐射器性能计算

在航天器热控制中，空间辐射器是最主要的排热部件。本文对双面及单面管道—楔形肋片式空间辐射器进行了详细的热分析，并完成了管道—楔形肋片式空间辐射器的性能计算     

资源一号卫星CCD相机辐射定标和图像辐射校正

文章介绍了CCD相机的定标概念,结合资源一号卫星多光谱CCD相机说明设计对定标手段设置的选择、定标机构的设计及操作要点、定标实验测试规划的重要作用,最后提出像校正方法的意见。     

星载数字电子设备的辐射加固技术(一)

对国外星载电子设备特别是常用的ＣＭＯＳ器件在空间环境下的抗辐射性能进行大量调研和长期跟踪，在此基础上总结了国外近年来对大规模集成电路辐射失效机理的研究成果，对比了各种器件工艺集成电路的抗辐射性能，重点分析了星载电子系统总剂量辐射损坏、单粒子翻转和单粒子锁定机理，针对这三种由空间辐射引起的星载电子系统失效这一特殊问题，分别介绍了国内外行之有效的辐射加固技术，最后提出了设计星载电子系统的一些建议。     

Xilinx SRAM型FPGA抗辐射设计技术研究

针对Xilinx SRAM型FPGA在空间应用中的可行性，分析了Xilinx SRAM型FPGA的结构，以及空间辐射效应对这种结构FPGA的影响，指出SRAM型的FPGA随着工艺水平的提高、器件规模的增大和核电压的降低，抗总剂量效应不断提高，抵抗单粒子效应，尤其是单粒子翻转和单粒子瞬态脉冲的能力降低。分析了FPGA综合后常见的Half-latch在辐射环境中的影响并结合实际工程实践给出了解决上述问题的一些有用办法和注意事项，如，冗余设计、同步设计、算术逻辑运算结果校验、白检等。最后还提出一种基于COTS器件的“由顶到底”的星载信号处理平台结构，分析了这种结构在抵抗辐射效应时的优势。有关FPGA抗辐射的可靠性设计方法已经在某卫星通信载道中成功应用，并通过了各种卫星环境试验，该技术可以为有关航天电子设备设计提供参考。     

空间用功率MOSFET器件2N7266总剂量

文章针对空间用功率MOSFET器件2N7266进行了60Co源γ射线辐射试验研究。在辐射过程中,采用JT-1型晶体管特性图示仪和计算机控制的摄像机实时监测器件电参数随辐射剂量变化的特征,通过试验研究获得了被试器件阈值电压、漏电流和击穿电压随总剂量变化的特征,得出了被试器件抗总剂量辐射的指标。研究结果可为被试器件在航天器型号的使用提供技术参考依据。     

宇航用双极器件和光电耦合器位移损伤试验研究

文章针对器件的位移损伤效应,利用质子加速器产生的质子及反应堆中子对化合物器件和硅器件位移损伤进行试验研究,得到了GaAs光电耦合器的电流传输比(CTR)和硅晶体管电流增益hFE的退化率随等效剂量的变化规律。研究结果表明,在质子70 MeV以上高能量范围,对于硅器件适用的位移损伤等效原理对于GaAs化合物器件则不再适用,需要修正。根据试验数据,给出了经验的修正系数。     

辐射换热对平板气膜冷却性能影响

为了分析辐射换热对平板气膜冷却性能的影响,分别对不考虑辐射换热(耦合计算)与考虑辐射换热两种条件下的平板隔热屏进行了三维流热耦合数值模拟研究,并与绝热壁(不考虑隔热屏固壁导热)的计算结果进行了对比。辐射换热采用离散坐标法。得到了3种不同主/次流总温比(Rt)条件下气膜冷却效果、流场、单位面积冷流体热负荷以及流量系数的对比结果与变化规律。结果表明:气膜冷却效果沿流向逐渐降低,且随总温比的增加而降低;在展向上气膜冷却效果呈现中间高两边低的分布规律,最大与最小相对值在绝热壁条件下达到最大,为94.5%,辐射换热次之,为13.5%,不考虑辐射换热时最小,为9.8%。与不考虑辐射换热结果相比,辐射换热对气膜冷却效果的影响在流动方向逐渐变大,气膜孔附近展向温度梯度增大,冷流体热负荷增加了92.8%,二者计算的流量系数相差不大,为1.1%,与绝热壁计算结果相比,流量系数减小了13.1%。随着总温比增加流量系数减小,最大值与最小值相差不大,为1.1%。     

Clouds and Earth Radiant Energy System (CERES), a review: Past,present and future

The Clouds and Earth Radiant Energy System (CERES) project’s objectives are to measure the reflected solar radiance (shortwave) and Earth-emitted (longwave) radiances and from these measurements to compute the shortwave and longwave radiation fluxes at the top of the atmosphere (TOA) and the surface and radiation divergence within the atmosphere. The fluxes at TOA are to be retrieved to an accuracy of 2%. Improved bidirectional reflectance distribution functions (BRDFs) have been developed to compute the fluxes at TOA from the measured radiances with errors reduced from ERBE by a factor of two or more. Instruments aboard the Terra and Aqua spacecraft provide sampling at four local times. In order to further reduce temporal sampling errors, data are used from the geostationary meteorological satellites to account for changes of scenes between observations by the CERES radiometers.     

Trapped proton fluxes measured on board LEO satellites in comparison with models

The proton fluxes from the low-Earth orbital satellites databases (NPOES-17 and CORONAS-F) were analyzed for the quiet geomagnetic period in April 2005. The satisfactory consent was found between the experimental and the AP8 model fluxes of the trapped protons with energy more than ∼10 MeV. At the same time, trapped proton fluxes with energy less than 10 MeV measured by LEO satellites were higher than the ones predicted by the AP8 model in the region of the SAA (drift shell L < 1.5).     

Solar cycle variation of “killer” electrons at geosynchronous orbit and electron flux correlation with the solar wind parameters and ULF waves intensity

To construct models for hazard prediction from radiation belt particles to satellite electronics, one should know temporal behavior of the particle fluxes. We analyzed 11-year variation in relativistic electron flux (E>2 MeV) at geosynchronous orbit using measurements made by GOES satellites during the 23rd sunspot cycle. As it is believed that electron flux enhancements are connected with the high-speed solar wind streams and ULF or/and VLF activity in the magnetosphere, we studied also solar cycle changes in rank order cross-correlation of the outer radiation belt electron flux with the solar wind speed and both interplanetary and on-ground wave intensity. Data from magnetometers and plasma sensors onboard the spacecraft ACE and WIND, as well as magnetic measurements at two mid-latitude diametrically opposite INTERMAGNET observatories were used. Results obtained show that average value of relativistic electron flux at the decay and minimum phases of solar activity is one order higher than the flux during maximum sunspot activity. Of all solar wind parameters, only solar wind speed variation has significant correlation with changes in relativistic electron flux, taking the lead over the latter by 2 days. Variations in ULF amplitude advance changes in electron flux by 3 days. Results of the above study may be of interest for model makers developing forecast algorithms.