基于一维相控阵引信的起爆控制算法研究

工程上实现最佳引战配合要求导弹战斗部最大破片密度方向瞄准目标要害部位。基于一维相控阵引信的波束控制技术,推导了最佳起爆角和起爆延时算法,并研究了一种改进卡尔曼滤波方法在此算法中的应用。该滤波算法将球坐标系中导弹导引头的测量信息转换到直角坐标系下进行滤波,同时消除了由于坐标转换而引起的偏差。仿真结果表明,该滤波算法的应用能得到很高的最佳起爆角和起爆延时估计精度。     

太阳微波爆发精细结构与硬X射线耀斑的相关

北京天文台在２．８４ＧＨｚ频率上观测到的带短时标精细结构的微波爆发与日本ＹＯＨＫＯＨ卫星上ＨＸＴ在１９９１年１０月－１９９２年１２月观测到的硬Ｘ射线爆发（ＨＸＢ）事件作了比较，发现在２０个微波精细结构爆发事件只有１２个与ＹＯＨＫＯＨ卫星记录的ＨＸＢ有对应关系．本文对１９９２年６月７日典型事件中２．８４ＧＨｚ与ＨＸＢ共同存在的百秒量级的准周期振荡作了分析及源区参数的计算，并作了简要的讨论．     

机身前体横截面形状对三角翼涡破裂位置的影响

通过求解三维定常雷诺时均方程,采用剪切应力输运(SST)湍流模型,在亚声速范围内,分别对融合体前体-三角翼组合体和旋成体前体-三角翼组合体流场中翼涡破裂现象进行了数值模拟.模拟结果显示:与旋成体前体相比,在中、大迎角时,融合体前体的分离涡,涡量集中、强度高,进入机翼上方流场后,能够与翼涡密切耦合,彻底地改变翼涡强度的分...     

APU 转子爆破对防火墙影响的研究

APU是安装在民用飞机上的辅助动力装置,是飞机上重要的部件,因此必须考虑APU 转子爆破时小碎片对飞机安全的影响。通过有限元软件LS-DYNA,分别模拟了APU 转子爆破时小碎片对APU 防火墙以及3种不同厚度加强板的冲击计算。根据数值计算结果,选择合适的加强板方案,既能防止防火墙碰撞区被小碎片击穿,同时付出的重量代价又较小。通过对APU 防火墙增加加强板,确保APU 转子爆破时飞机的安全 性,满足AC20-128A 的设计要求。     

温度场对航空发动机转子超转破裂的影响

CCAR33.27超转适航要求,分析和试验确定的超转转速,必须基于温度和温度梯度的最不利组合。因此,研究温度和温度梯度对超转破裂的影响有非常重要的意义。以某型航空发动机低压6级涡轮转子为例,采用极限应变方法开展了转子部件的超转破裂分析,对比了常温和高温（红线转速对应的温度分布）下转子关键轮盘应变分布趋势和应变增长规律、预测的超转破裂的起始位置和破裂转速等轮盘超转特性;针对超转破裂分析,提出了在高温条件下,经过常温超转破裂试验验证的方法应用的有效性条件。低压涡轮转子的分析结果也显示,红线转速对应的温度状态下,轮盘超转破裂转速比常温下显著降低,而高温下材料屈服强度的大幅降低则是破裂转速下降的主要原因。     

厘米-分米波段Ⅲ型爆发的统计分析

统计分析了太阳第23周期间(2000年7月至2004年9月)在625~1500,MHz,2600~3800,MHz和5200~7600,MHz范围频谱仪观测到的Ⅲ型射电爆发. 给出了Ⅲ型爆发的分布、寿命、频率漂移率、偏振度和频率带宽. 结果显示, 频率漂移率和频率带宽的平均值随频率的增加而增大, 寿命和偏振度的平均值既不是常数也不是在宽频延伸上保持均匀不变的.最多的Ⅲ型爆发分布在625~3800,MHz范围内, 且随频率的增加而增多. 分析表明, 电子加速和能量释放地点主要是在分米波范围内, 这个频率范围的特征可能与分米波段上的磁位形有关, 并且与主耀斑地点附近磁重联区中的电子加速有关. 然而, 还有相当数量的Ⅲ型爆发发生在5200~7600,MHz范围内, 这个特征表明电子加速的地点是在一个日冕的宽范围中. 关于厘米relax-relax 分米波段Ⅲ型爆发的辐射机制最可能包含相干的等离子体辐射或电子回旋脉泽辐射过程.      

The origin of the prompt optical emission in GRB 060111B

The detection of a bright optical emission measured with good temporal resolution during the prompt phase makes GRB 060111B a rare event that is especially useful for constraining theories of the prompt optical emission. Comparing this burst with other GRBs with evidence of optical peaks, we find that the optical peak epoch (t_p) is anti-correlated with the high energy burst energetic assuming an isotropic energy release (E_iso) in agreement with Liang et al. (2009), and that the steeper is the post-peak afterglow decay, the less is the agreement with the correlation. GRB 060111B is among the latters and it does not match the correlation. The Cannonball scenario is also discussed and we find that this model cannot be excluded for GRB 060111B.     

一种提升近地小行星防御中拦截效率的方法

利用核爆直接炸毁小行星或改变小行星的轨道以避免其与地球相撞,是近地小行星防御最主要的手段之一。文章基于美国爱荷华州立大学的超高速小行星拦截器(HAIV)概念,提出一种将原撞击引导器改为长杆撞击器的方案,采用自主研发的欧拉型冲击动力学仿真软件NTS模拟长杆撞击器对小行星连续开坑的过程,并在仿真中加入能量源以模拟核爆装置在不同深度爆炸对小行星产生的偏转与破坏效应。研究结果表明,采用长杆撞击器并合理控制撞击速度,能够引导核爆装置进入更深的地下爆炸,从而更加高效地耦合核爆能量,提升偏转小行星或直接摧毁小行星的能力。     

用大面积源检定核应急机载/车载伽玛能谱仪

人工核素大面积源标准是核工业航测遥感中心等单位经过十余年研究建立的新型计量保障标准,使用该标准,可对监测核应急伽玛辐射环境的机载/车载伽玛能谱仪进行检定.使用大面积源标准检定,可以有效地弥补因机载/车载伽玛能谱仪系统的角响应影响因素复杂而难于模拟计算的缺陷,为监测核应急伽玛辐射环境的机载/车载伽玛能谱仪提供了量值传递的保障.本文介绍了大面积源检定的原理和技术方法.     

Investigating the Coronal Mass Ejections associated with DH type-II radio bursts and solar flares during the ascending phase of the solar cycle 24

We studied a set of 74 CMEs, with shedding the light on the halo-CMEs (HCMEs), that are associated with decametric – hectometric (DH) type-II radio bursts (1–16?MHz) and solar flares during the period 2008–2014. The events were classified into 3 groups (disk, intermediate, and limb events) based on their longitudinal distribution.We found that the events are mostly distributed around 15.32° and 15.97° at the northern and southern solar hemispheres, respectively. We found that there is a clear dependence between the longitude and the CME’s width, speed, acceleration, mass, and kinetic energy. For the CMEs’ widths, most of the events were HCMEs (～62%), while the partial HCMEs comprised ～35% and the rest of events were CMEs with widths less than 120°. For the CMEs’ speeds, masses, and kinetic energies, the mean values showed a direct proportionality with the longitude, in which the limb events had the highest speeds, the largest masses, and the highest kinetic energies. The mean peak flux of the solar flares for different longitudes was comparable, but the disk flares were more energetic. The intermediate flares were considered as gradual flares since they tended to last longer, while the limb flares were considered as impulsive flares since they tended to last shorter.A weak correlation (R?=?0.32) between the kinetic energy of the CMEs and the duration of the associated flares has been noticed, while there was a good correlation (R?=?0.76) between the kinetic energy of the CMEs and the peak flux of the associated flares. We found a fair correlation (R?=?0.58) between the kinetic energy of the CMEs and the duration of the associated DH type-II radio bursts.