直升机红外辐射的理论计算

选取了适当的理论计算方法,给出了计算公式和计算步骤,进而在所假设的飞行状态下计算了直升机的红外辐射,包括直升机发动机的排气管辐射和直升机蒙皮辐射的全辐射量和红外波段辐射量,最后对计算结果进行了分析。从分析来看,计算结果是可信的。     

电子直线加速器辐射场优化的蒙特卡洛模拟

提供了一种用于设计医用电子直线加速器（1inac）X射线均整过滤器的方法,并将其用于电子束辐射系统的优化过程之中。采用MonteCarlo模拟计算方法,提供了2个真实的国产医用电子直线加速器的辐射研究成果：BJ-20加速器的15MVX射线辐射系统和BJ-14加速器的12MeV电子柬辐射系统。使用传统方法对上述成果进行了验证。     

单边膨胀喷管气动和红外辐射特性数值研究

通过计算流体动力学/红外辐射(CFD/IR)数值模拟的方法,研究了单膨胀边倾角、喉道高度、侧壁长度和落压比(NPR)对单边膨胀喷管(SERN)气动性能和红外辐射特性的影响.研究结果表明:轴向推力系数随着单膨胀边倾斜角度增大而急剧减小,推力矢量角随着单膨胀边倾斜角度增大而增大;随着喷管落压比的增大,轴向推力系数先增大后减小,推力矢量角减小;随着喷管侧壁长度的增加,轴向推力系数可略微提高;单膨胀边对尾焰和喷管内壁有显著的遮挡作用,喷管下方的整体红外辐射仅为上方的10%左右;随着喷管落压比的增加,喷管上方的整体红外辐射降低.      

紫外、真空紫外光谱辐射亮度标定技术

文章论述了紫外辐照对航天器敏感表面的破坏,并从原理上和方法上介绍了紫外、真空紫外光谱辐射亮度的3种标定技术.     

卫星抗强激光辐射效应模拟和评估技术

文章介绍了国外激光武器的研究以及对卫星抗激光辐射加固技术的重视,分析了激光作用的机理,提出了研究卫星抗强激光辐射效应模拟和评估的方法.     

卫星用光纤陀螺三轴组合的关键技术

研究了空间环境对光纤陀螺各项指标的影响,设计了一种新颖的卫星用光纤陀螺三轴组合.针对空间辐射、温度循环和真空环境对光纤陀螺的影响进行了模拟实验,通过分析实验数据得到了空间环境对光纤陀螺主要参数的影响机理.利用最小二乘滤波的方法建立了偏置误差模型,利用查表法建立了标度因数误差模型,并用现场可编程门阵列(FPGA)实时进行零偏和标度因数补偿,补偿后陀螺输出零偏稳定性为0.1(°)/h.同时详细分析了陀螺在空间低角速度环境下产生死区的原因,并利用周期相位扰动调制的方法消除了死区.在卫星用光纤陀螺三轴组合的设计中,实现了光源复用和冗余、空间主动和被动防护措施、在轨故障诊断等技术.      

涡轮风扇发动机在飞机红外隐身上的优势

简要介绍了飞机红外隐身技术的发展现状,比较详细地阐述了涡扇发动机在飞机红外隐身上的优势,如可降低发动机及其尾焰的红外辐射强度;兼顾了良好的隐身性能和很好的作战性、机动性.     

超声波辐照对聚合物及其复合材料性能的影响

综述了超声辐照对聚合物及其复合材料在超细添加材料分散、力学性能、理化性能以及组织结构等方面的影响规律及其相应的作用机理,提出了超声波辐照工艺与其他工艺复合等的发展趋势和应用前景。     

Solar physics with the Square Kilometre Array

The Square Kilometre Array (SKA) will be the largest radio telescope ever built, aiming to provide collecting area larger than 1?km². The SKA will have two independent instruments, SKA-LOW comprising of dipoles organized as aperture arrays in Australia and SKA-MID comprising of dishes in South Africa. Currently the phase-1 of SKA, referred to as SKA1, is in its late design stage and construction is expected to start in 2020. Both SKA1-LOW (frequency range of 50–350?MHz) and SKA1-MID Bands 1, 2, and 5 (frequency ranges of 350–1050, 950–1760, and 4600–15,300?MHz, respectively) are important for solar observations. In this paper we present SKA’s unique capabilities in terms of spatial, spectral, and temporal resolution, as well as sensitivity and show that they have the potential to provide major new insights in solar physics topics of capital importance including (i) the structure and evolution of the solar corona, (ii) coronal heating, (iii) solar flare dynamics including particle acceleration and transport, (iv) the dynamics and structure of coronal mass ejections, and (v) the solar aspects of space weather. Observations of the Sun jointly with the new generation of ground-based and space-borne instruments promise unprecedented discoveries.     

Flight safety implications of the extreme solar proton event of 23 February 1956

There is considerable speculation about the effects at aircraft altitudes resulting from extreme solar proton events. The ground level event (GLE) of 23 February 1956 (GLE 5), remains the largest solar proton event of the neutron monitor era in terms of its influence on count rates at monitors near sea level. During this GLE the count rate was increased by as much as 4760% (15-min average) at the Leeds monitor relative to the count rate from galactic cosmic radiation (GCR). Two modern models of the event cumulative solar proton spectrum for this event, a 6-parameter fit in energy and a 4-parameter Band fit in rigidity, are compared with 1-h of GCR at solar minimum. While effective doses calculated with CARI-7A for both models at low geomagnetic cutoff rigidities are indeed high when compared with GCR and can exceed recommended exposure limits, both GLE spectra exhibit a much stronger dependence on cutoff rigidity than GCR, and a larger fraction of the dose from neutrons. At locations with cutoff rigidities above 4.2 and 6.4?GV, respectively, the GLE effective doses are smaller than the GCR hourly dose. At locations with cutoff rigidities above about 4?GV, GCR was the dominant source of exposure in 10?h or less at all altitudes examined. This suggests that if a similar event occurs in the future, low- and mid-latitude flights at modern jet flight altitudes could be well-protected by Earth’s magnetic field.