CCSDS邻近空间链路协议的初步探究

介绍了空间数据系统咨询委员会(CCSDS)制定的邻近空间链路协议的产生背景及发展现状.     

1+1/2对转涡轮可调高压导叶流场及损失的数值研究

调节高压导叶开度可以有效控制1+1/2对转涡轮流量,同时导叶的调节也伴随着一些附加损失的产生,为了使采用可调导叶获得的效益不被涡轮效率的下降抵消过多,有必要对可调导叶的流场及间隙流动进行详细的分析。通过数值研究表明,当采用可调导叶端部加入间隙后,在上下两端壁附近会出现高损失区。间隙泄漏流除了进口端壁的来流之外,还有一部分来自于叶片压力面的附面层,使得压力面出现明显的展向二次流。泄漏流的流量越大越容易形成泄漏涡,压力面和吸力面之间的压差是泄漏涡形成的主要动力。     

TA1/Q235循环累积变形复合界面研究

借助扫描电镜、X射线衍射仪等手段,对循环累积变形复合后的Ti/Q235复合试样的界面生成物和界面形貌进行分析.结果表明:两母材元素在界面反应生成TiC和Fe2Ti化合物;TA1/Q235复合前去除氧化膜后在待结合面上制造一层脆性覆膜,有利于形成冶金结合.     

考虑冷气的多级涡轮翘曲S1流面的气动优化

为了缩短涡轮气动设计的周期,进一步发掘涡轮叶型的改进潜力,搭建了多级涡轮的翘曲S1流面气动优化平台.该平台具有速度快,周期短的特点.在考虑冷气的前提下,对多级叶片进行多层并行优化,避免了单列优化后叶列间匹配差的缺点,同时克服了多层S1流面的气动效率此消彼长的缺陷.对某型两级高压涡轮进行了气动优化设计,优化后10%,50%,90%叶高的S1流面的考虑冷气的气动效率分别提高了0.569%,0.490%,0.405%;第1级和第2级考虑冷气的气动效率分别提高了0.18%,0.05%;涡轮整体气动效率提高了0.15%;优化效果明显.经过分析可知,优化有效减小第1级导叶的通道横向二次流损失和第1级动叶的激波损失,第2级的原始叶型设计较为合理.下端壁喷射冷气是降低S1流面优化有效性的重要原因.     

离港航空器滑出时间的BP神经网络预测模型

准确地预测离港航空器滑出时间可有效提升机场场面运行效率,降低运行成本。构建基于BP 神经网络的离港航空器滑出时间预测模型,分析影响离港航空器滑出时间的可量化因素,并对其相关性进行检验;通过我国中南某机场2 周实际运行数据对模型进行验证,并以均方根误差、平均绝对误差和平均绝对误差百分比检验预测结果的准确性。结果表明：同时...     

高能合成煤油GN-1性能研究

为了获得高能合成煤油（GN-1煤油）物化性能随温度和压力的变化规律,掌握GN-1煤油与现役火箭煤油在应用特性方面的差异,采用理论计算和实验方法,对GN-1煤油在物化性能（密度、黏度、定压比热容、导热系数、表面张力）变化规律、安全特性（闪点、自燃温度、燃点、爆炸极限、毒性）、流动传热与结焦特性以及点火延迟特性进行了研究,并与火箭煤油进行了对比。通过实验研究得到了最高温度不超过200℃,最高压力不超过25MPa下GN-1煤油的密度、黏度、定压比热容、导热系数、表面张力实验数据,结合理论计算,获得了GN-1煤油在-40~350℃,0.1~60MPa内热物性变化规律,并与火箭煤油进行了对比。此外,研究结果还表明：GN-1煤油的闪点为40℃（低于火箭煤油闪点74℃）,自燃温度为305℃（高于火箭煤油自燃温度225℃）,燃点为47℃（低于火箭煤油燃点82℃）,爆炸极限为0.44%～2.9%（40℃）,GN-1煤油和火箭煤油急性经口毒性LD₅₀＞5000mg/kg。在入口压力10MPa,流速10m/s,内壁温480℃条件下,GN-1煤油的传热系数比火箭煤油提高14.4%。在采用GH3128高温合金管条件下,GN-1煤油出口油温220℃时试验段平均结焦速率是出口油温150℃时的4.43倍,GN-1煤油316L不锈钢管路中试验段平均结焦速率为GH3128高温合金管路中的22.3%。在970～1105K内,GN-1煤油的点火延迟时间为火箭煤油的55.6%～69.3%。     

一种电离层垂直剖面物理模型及其与IRI-90模型的比较

在80-500km范围内考虑了3种中性成份的4种离子,从严格的电子和离子密度连续方程出发,对中性风和扩散效应进行了全面、连续的考虑,由此建立了一种电离层的物理模式;在此模式的基础上针对北京地区分别对太阳活动低年(F_10.7=60)、高年(F_10.7=300)的春(DOY=90)、夏(DOY=180)、秋(DOY=270)、冬(DOY=365)进行计算,并将所得结果与IRI-90进行了比较.结果表明: E层为典型的Chapman层: E-F谷区深度一般为0.2-0.5之间,比IRI要深;F₁缘在太阳活动低年的四季都出现,其中夏天最明显,已形成了一个F₁层,冬天最不明显,仅表现为一个轻微的凸缘,在太阳活动高年只有夏天出现了F₁凸缘,这与现有理论相符合,而IRI-90较少出现明显的F₁缘;F₂层的电子密度是活动高年比低年大,平均冬天比夏天大,这与观测结果也基本符合.      

民用航空发动机振动配平功能设计

振动故障是航空发动机常见并且危害较大的故障,可能导致发动机运营事故或提前更换,增加航空公司运营成本,进行转子平衡是降低发动机振动的重要措施。根据民用涡扇发动机的设计特点和振动配平相关原理,设计了利用EVMU进行发动机振动配平计算的功能,并通过试验进行了验证。试验结果表明:采用根据EVMU计算出的方案配平发动机,能够有效地降低发动机N1振动值,满足航线使用需求。     

Science objectives of the magnetic field experiment onboard Aditya-L1 spacecraft

The Aditya-L1 is first Indian solar mission scheduled to be placed in a halo orbit around the first Lagrangian point (L1) of Sun-Earth system in the year 2018–19. The approved scientific payloads onboard Aditya-L1 spacecraft includes a Fluxgate Digital Magnetometer (FGM) to measure the local magnetic field which is necessary to supplement the outcome of other scientific experiments onboard. The in-situ vector magnetic field data at L1 is essential for better understanding of the data provided by the particle and plasma analysis experiments, onboard Aditya-L1 mission. Also, the dynamics of Coronal Mass Ejections (CMEs) can be better understood with the help of in-situ magnetic field data at the L1 point region. This data will also serve as crucial input for the short lead-time space weather forecasting models.The proposed FGM is a dual range magnetic sensor on a 6?m long boom mounted on the Sun viewing panel deck and configured to deploy along the negative roll direction of the spacecraft. Two sets of sensors (tri-axial each) are proposed to be mounted, one at the tip of boom (6?m from the spacecraft) and other, midway (3?m from the spacecraft). The main science objective of this experiment is to measure the magnitude and nature of the interplanetary magnetic field (IMF) locally and to study the disturbed magnetic conditions and extreme solar events by detecting the CME from Sun as a transient event. The proposed secondary science objectives are to study the impact of interplanetary structures and shock solar wind interaction on geo-space environment and to detect low frequency plasma waves emanating from the solar corona at L1 point. This will provide a better understanding on how the Sun affects interplanetary space.In this paper, we shall give the main scientific objectives of the magnetic field experiment and brief technical details of the FGM onboard Aditya-1 spacecraft.     

Evaluation of the improvement of IRI-2016 over IRI-2012 at the India low-latitude region during the ascending phase of cycle 24

This paper investigated the performance of the latest International Reference Ionosphere model (IRI-2016) over that of IRI-2012 in predicting total electron content (TEC) at three different stations in the Indian region. The data used were Global Positioning System (GPS) data collected during the ascending phase of solar cycle 24 over three low-latitude stations in India namely; Bangalore (13.02°N Geographic latitude, 77.57°E Geographic longitude), Hyderabad (17.25°N Geographic latitude, 78.30°E Geographic longitude) and Surat (21.16°N Geographic latitude, 72.78°E Geographic longitude). Monthly, the seasonal and annual variability of GPS-TEC have been compared with those derived from International Reference Ionosphere IRI-2016 and IRI-2012 with two different options of topside electron density: NeQuick and IRI01-corr. It is observed that both versions of IRI (i.e., IRI-2012 and IRI-2016) predict the GPS-TEC with some deviations, the latest version of IRI (IRI-2016) predicted the TEC similar to those predicted by IRI-2012 for all the seasons at all stations except for morning hours (0500 LT to 1000?LT). This shows that the effect of the updated version is seen only during morning hours and also that there is no change in TEC values by IRI-2016 from those predicted by IRI-2012 for the rest of the time of the day in the Indian low latitude region. The semiannual variations in the daytime maximum values of TEC are clearly observed from both GPS and model-derived TEC values with two peaks around March-April and September-October months of each year. Further, the Correlation of TEC derived by IRI-2016 and IRI-2012 with EUV and F10.7 shows similar results. This shows that the solar input to the IRI-2016 is similar to IRI 2012. There is no significant difference observed in TEC, bottom-side thickness (B0) and shape (B1) parameter predictions by both the versions of the IRI model. However, a clear improvement is visible in hmF2 and NmF2 predictions by IRI-2016 to that by IRI-2012. The SHU-2015 option of the IRI-2016 gives a better prediction of NmF2 for all the months at low latitude station Ahmedabad compare to AMTB 2013.