猎鹰9号火箭发射及箭体复用的分析

猎鹰9号火箭截至2023年年底已完成286次发射。对猎鹰9号火箭特别是Block5版本火箭的发射情况进行了完整梳理统计,重点分析了一级箭体的复用情况以及发射、回收的相关能力保障,对火箭的经济性和未来前景作了预测。     

Internal fuselage noise: comparison of computations and tests on a Falcon airframe

An unequipped Falcon 2000 airframe, a complex heterogeneous structure reduced to the fuselage alone, was subjected to vibro-acoustic characterization within the framework of a cooperative effort by Aerospatiale, Dassault-Aviation, and Onera. Onera's Structural Dynamics and Coupled Systems Department measured the structure's vibro-acoustic responses for four mechanical excitation configurations, and analysed three structural configurations: fuselage alone without floor, with floor, and with floor and internal wall. The resulting database of vibratory and acoustic level measurements is used for validating numerical models in the low- and medium-frequency range, as well as statistical energy analysis (SEA) models in the medium- and high-frequency range.The database was analysed by Dassault-Aviation and Onera. We present here the computation/test comparisons and the limitations of the methods in use. All of the data and comparisons validate the predictive vibro-acoustic response models and methods for a Falcon fuselage subjected to a mechanical excitation.     

LC9材料S—N曲线的测定及数据处理

根据ＬＣ９疲劳试验情况，阐述了Ｓ－Ｎ曲线的测定、绘制及数据处理方法；简要介绍了ＬＣ９应力集中系数５的疲劳特征，及在指定寿命（Ｎ＝１０＾７）下的条件平均疲劳极限值。     

直9直升机机载数据传输电缆电磁耦合分析

通过对数据传输电缆的仿真分析计算,得到了传输信号频率、电缆回路之间的距离与电磁耦合之间的关系.对于直9系列直升机中数据传输电缆的物理模型计算结果表明,感应电压会在传输频率为75MHz时达到最大值,线间距离为1.5mm时具有最小值.分析结果为直9系列直升机/飞机机载数据电缆的布线优化和电磁兼容改进设计提供一定参考依据.     

The Coma of Comet 9P/Tempel 1

As comet 9P/Tempel 1 approaches the Sun in 2004–2005, a temporary atmosphere, or “coma,” will form, composed of molecules and dust expelled from the nucleus as its component icy volatiles sublimate. Driven mainly by water ice sublimation at surface temperatures T > 200 K, this coma is a gravitationally unbound atmosphere in free adiabatic expansion. Near the nucleus (≤ 10² km), it is in collisional equilibrium, at larger distances (≥10⁴ km) it is in free molecular flow. Ultimately the coma components are swept into the comet’s plasma and dust tails or simply dissipate into interplanetary space. Clues to the nature of the cometary nucleus are contained in the chemistry and physics of the coma, as well as with its variability with time, orbital position, and heliocentric distance. The DI instrument payload includes CCD cameras with broadband filters covering the optical spectrum, allowing for sensitive measurement of dust in the comet’s coma, and a number of narrowband filters for studying the spatial distribution of several gas species. DI also carries the first near-infrared spectrometer to a comet flyby since the VEGA mission to Halley in 1986. This spectrograph will allow detection of gas emission lines from the coma in unprecedented detail. Here we discuss the current state of understanding of the 9P/Tempel 1 coma, our expectations for the measurements DI will obtain, and the predicted hazards that the coma presents for the spacecraft. An erratum to this article is available at .     

Deep Impact Mission Design

The Deep Impact mission is designed to provide the first opportunity to probe below the surface of a comet nucleus by a high-speed impact. This requires finding a suitable comet with launch and encounter conditions that allow a meaningful scientific experiment. The overall design requires the consideration of many factors ranging from environmental characteristics of the comet (nucleus size, dust levels, etc.), to launch dates fitting within the NASA Discovery program opportunities, to launch vehicle capability for a large impactor, to the observational conditions for the two approaching spacecraft and for telescopes on Earth.     

The History and Dynamics of Comet 9P/Tempel 1

Since its discovery in 1867, periodic comet 9P/Tempel 1 has been observed at 10 returns to perihelion, including all its returns since 1967. The observations for the seven apparitions beginning in 1967 have been fit with an orbit that includes only radial and transverse nongravitational accelerations that model the rocket-like thrusting introduced by the outgassing of the cometary nucleus. The successful nongravitational acceleration model did not assume any change in the comet’s ability to outgas from one apparition to the next and the outgassing was assumed to reach a maximum at perihelion. The success of this model over the 1967–2003 interval suggests that the comet’s spin axis is currently stable. Rough calculations suggest that the collision of the impactor released by the Deep Impact spacecraft will not provide a noticeable perturbation on the comet’s orbit nor will any new vent that is opened as a result of the impact provide a noticeable change in the comet’s nongravitational acceleration history. The observing geometries prior to, and during, the impact will allow extensive Earth based observations to complement the in situ observations from the impactor and flyby spacecraft.     

九自由度运动模拟器相对位置精度分析与指标分解

摘要： 九自由度运动模拟器是标定航天器交会对接GNC子系统中交会对接光学成像敏感器（CRDS）的关键设备,具有较高的相对位置精度要求.以此为出发点,对影响系统综合指标的误差组成进行系统性分析.梳理各误差分量的关系及相互作用原理,建立误差模型,通过对系统综合指标进行合理的分解与分配,最终使九自由度运动模拟器系统精度达到设计要求.     

等离子喷涂LaTi2Al9O19热障涂层的微观组织结构及热物理性能

 第一代热障涂层(TBCs)由氧化钇部分稳定的氧化锆(YSZ)陶瓷隔热层和金属粘结层组成,该涂层长期使用温度低于1 200℃。随着先进航空发动机向着高推重比发展,迫切要求发展新一代超高温、高隔热热障涂层材料。LaTi₂Al₉O₁₉(LTA)在1 500℃长期保持相稳定,是一种非常有前景的超高温热障涂层候选材料。本文采用大气等离子喷涂(APS)制备了LTA涂层,研究了喷涂工艺对涂层微观组织结构和热物理性能的影响。结果表明沉积态涂层中含少量的非晶态,在860℃和1 130℃出现晶化峰。等离子喷涂过程中La₂O₃挥发量较多,导致沉积态涂层中La元素与原始粉末相比含量偏低,而其他组分的化学成分随喷涂功率变化不大。LTA涂层的热扩散系数在1 400℃下为0.3~0.4 mm²·s^-1,热导率为1.1~1.6 W·m^-1·K^-1。1 050℃经过20小时热处理后,得到晶化的涂层在晶化温度范围内的热扩散系数和热导率值均增大。随着喷涂功率减小,涂层孔隙率增加,热导率减小。     

The primordial Helium-4 abundance determination: systematic effects

By extrapolating to O/H = N/H = 0 the empirical correlations Y–O/H and Y–N/H defined by a relatively large sample of 45 Blue Compact Dwarfs (BCDs), we have obtained a primordial ⁴Helium mass fraction Y _p=0.2443±0.0015 with dY/dZ=2.4±1.0. This result is in excellent agreement with the average Y _p=0.2452±0.0015 determined in the two most metal-deficient BCDs known, I Zw 18 (Z /50) and SBS 0335–052 (Z /41), where the correction for He production is smallest. The quoted error (1) of 1% is statistical and does not include systematic effects. We examine various systematic effects including collisional excitation of hydrogen lines, ionization structure and temperature fluctuation effects, and underlying stellar Hei absorption, and conclude that combining all systematic effects, our Y _p may be underestimated by 2–4%. Taken at face value, our Y _p implies a baryon-to-photon number ratio =(4.7^+1.0 _–0.8)×10^–10 and a baryon mass fraction _b h ² ₁₀₀=0.017±0.005 (2), consistent with the values obtained from deuterium and Cosmic Microwave Background measurements. Correcting Y _p upward by 2–4% would make the agreement even better.