“通过式反射线”:一种校准双六端口自动网络分析仪的改进技术

在一篇较早的论文中,曾经叙述过采用“通过式短路延迟线”(TSD)来校准双六端口自动网络分析仪的技术。另外一种方案只需要一节精密传输线和一个“校准电路”。目前已把这两种略有不同途径的优点结合起来,而不再需要已知短路或者“校准电路”。本文将就这种新方法,做理论探讨。     

基于微服务架构的智能数控系统

提出了一种基于微服务架构的开放式智能数控系统体系结构,构建了基于微服务架构的数控系统设计技术框架。采用领域驱动设计思想,将数控系统拆分为一系列松散耦合、独立部署的微服务,从而提高可重构、可扩展性,将颤振抑制等智能功能封装在微服务中,实现热插拔式的集成,并进行叶轮切削试验。结果表明,微服务架构的智能数控系统具有良好的动态扩展和可重构性,并且加载颤振抑制微服务后可有效提高表面质量。     

复合材料缠绕后置处理方法研究

利用芯模表面的离散落纱点,依据空间几何和微分几何理论,针对纤维缠绕过程提出纤维缠绕出纱点轨迹的网格后置处理方法。该方法首先通过纤维缠绕轨迹的落纱点,以及缠绕过程中等悬纱长约束条件来求取出纱点,然后通过计算相邻出纱点的各坐标差得到机床运动轨迹,最后分别通过对三通管和组合回转体的缠绕成型实验,来验证该网格后置处理方法在处理非回转体和回转体缠绕出纱点轨迹的可行性和准确性。     

M stars as targets for terrestrial exoplanet searches and biosignature detection

The changing view of planets orbiting low mass stars, M stars, as potentially hospitable worlds for life and its remote detection was motivated by several factors, including the demonstration of viable atmospheres and oceans on tidally locked planets, normal incidence of dust disks, including debris disks, detection of planets with masses in the 5-20 M() range, and predictions of unusually strong spectral biosignatures. We present a critical discussion of M star properties that are relevant for the long- and short-term thermal, dynamical, geological, and environmental stability of conventional liquid water habitable zone (HZ) M star planets, and the advantages and disadvantages of M stars as targets in searches for terrestrial HZ planets using various detection techniques. Biological viability seems supported by unmatched very long-term stability conferred by tidal locking, small HZ size, an apparent short-fall of gas giant planet perturbers, immunity to large astrosphere compressions, and several other factors, assuming incidence and evolutionary rate of life benefit from lack of variability. Tectonic regulation of climate and dynamo generation of a protective magnetic field, especially for a planet in synchronous rotation, are important unresolved questions that must await improved geodynamic models, though they both probably impose constraints on the planet mass. M star HZ terrestrial planets must survive a number of early trials in order to enjoy their many Gyr of stability. Their formation may be jeopardized by an insufficient initial disk supply of solids, resulting in the formation of objects too small and/or dry for habitability. The small empirical gas giant fraction for M stars reduces the risk of formation suppression or orbit disruption from either migrating or nonmigrating giant planets, but effects of perturbations from lower mass planets in these systems are uncertain. During the first approximately 1 Gyr, atmospheric retention is at peril because of intense and frequent stellar flares and sporadic energetic particle events, and impact erosion, both enhanced, the former dramatically, for M star HZ semimajor axes. Loss of atmosphere by interactions with energetic particles is likely unless the planetary magnetic moment is sufficiently large. For the smallest stellar masses a period of high planetary surface temperature, while the parent star approaches the main sequence, must be endured. The formation and retention of a thick atmosphere and a strong magnetic field as buffers for a sufficiently massive planet emerge as prerequisites for an M star planet to enter a long period of stability with its habitability intact. However, the star will then be subjected to short-term fluctuations with consequences including frequent unpredictable variation in atmospheric chemistry and surficial radiation field. After a review of evidence concerning disks and planets associated with M stars, we evaluate M stars as targets for future HZ planet search programs. Strong advantages of M stars for most approaches to HZ detection are offset by their faintness, leading to severe constraints due to accessible sample size, stellar crowding (transits), or angular size of the HZ (direct imaging). Gravitational lensing is unlikely to detect HZ M star planets because the HZ size decreases with mass faster than the Einstein ring size to which the method is sensitive. M star Earth-twin planets are predicted to exhibit surprisingly strong bands of nitrous oxide, methyl chloride, and methane, and work on signatures for other climate categories is summarized. The rest of the paper is devoted to an examination of evidence and implications of the unusual radiation and particle environments for atmospheric chemistry and surface radiation doses, and is summarized in the Synopsis. We conclude that attempts at remote sensing of biosignatures and nonbiological markers from M star planets are important, not as tests of any quantitative theories or rational arguments, but instead because they offer an inspection of the residues from a Gyr-long biochemistry experiment in the presence of extreme environmental fluctuations. A detection or repeated nondetections could provide a unique opportunity to partially answer a fundamental and recurrent question about the relation between stability and complexity, one that is not addressed by remote detection from a planet orbiting a solar-like star, and can only be studied on Earth using restricted microbial systems in serial evolution experiments or in artificial life simulations. This proposal requires a planet that has retained its atmosphere and a water supply. The discussion given here suggests that observations of M star exoplanets can decide this latter question with only slight modifications to plans already in place for direct imaging terrestrial exoplanet missions.     

Interplanetary transfer of photosynthesis: an experimental demonstration of a selective dispersal filter in planetary island biogeography

We launched a cryptoendolithic habitat, made of a gneissic impactite inoculated with Chroococcidiopsis sp., into Earth orbit. After orbiting the Earth for 16 days, the rock entered the Earth's atmosphere and was recovered in Kazakhstan. The heat of entry ablated and heated the rock to a temperature well above the upper temperature limit for life to below the depth at which light levels are insufficient for photosynthetic organisms ( approximately 5 mm), thus killing all of its photosynthetic inhabitants. This experiment shows that atmospheric transit acts as a strong biogeographical dispersal filter to the interplanetary transfer of photosynthesis. Following atmospheric entry we found that a transparent, glassy fusion crust had formed on the outside of the rock. Re-inoculated Chroococcidiopsis grew preferentially under the fusion crust in the relatively unaltered gneiss beneath. Organisms under the fusion grew approximately twice as fast as the organisms on the control rock. Thus, the biologically destructive effects of atmospheric transit can generate entirely novel and improved endolithic habitats for organisms on the destination planetary body that survive the dispersal filter. The experiment advances our understanding of how island biogeography works on the interplanetary scale.     

Biomarker response to galactic cosmic ray-induced NOx and the methane greenhouse effect in the atmosphere of an Earth-like planet orbiting an M dwarf star

Planets orbiting in the habitable zone of M dwarf stars are subject to high levels of galactic cosmic rays (GCRs), which produce nitrogen oxides (NOx) in Earth-like atmospheres. We investigate to what extent these NO(Mx) species may modify biomarker compounds such as ozone (O3) and nitrous oxide (N2O), as well as related compounds such as water (H2O) (essential for life) and methane (CH4) (which has both abiotic and biotic sources). Our model results suggest that such signals are robust, changing in the M star world atmospheric column due to GCR NOx effects by up to 20% compared to an M star run without GCR effects, and can therefore survive at least the effects of GCRs. We have not, however, investigated stellar cosmic rays here. CH4 levels are about 10 times higher on M star worlds than on Earth because of a lowering in hydroxyl (OH) in response to changes in the ultraviolet. The higher levels of CH4 are less than reported in previous studies. This difference arose partly because we used different biogenic input. For example, we employed 23% lower CH4 fluxes compared to those studies. Unlike on Earth, relatively modest changes in these fluxes can lead to larger changes in the concentrations of biomarker and related species on the M star world. We calculate a CH4 greenhouse heating effect of up to 4K. O3 photochemistry in terms of the smog mechanism and the catalytic loss cycles on the M star world differs considerably compared with that of Earth.     

Homochirality in an early peptide world

A recently proposed model of non-autocatalytic reactions in dipeptide formation that leads to spontaneous symmetry breaking and homochirality was examined. The model is governed by activation, polymerization, epimerization, and depolymerization of amino acids. Symmetry breaking was determined to result primarily from the different rates of reactions that involve homodimers and heterodimers, i.e., stereoselective reactions, and the fact that epimerization can only occur on the N-terminal residue and not on the C-terminal residue. This corresponds to an auto-inductive cyclic process that works only in one direction. It is argued that epimerization mimics autocatalytic behavior as well as mutual antagonism, both of which are known to be crucial for the production of full homochirality.     

纤维缠绕/辅带/铺丝成型设备的发展状况

目前,飞机复材构件的自动化成型工艺主要包括纤维缠绕、纤维带铺放和纤维丝铺放3种类型.其中,纤维缠绕技术是最早开发并广泛使用的加工技术,亦是最成熟的生产技术.     

ZrO2基热障涂层陶瓷材料研究进展

由于ZrO2基陶瓷材料在热障涂层上的广泛应用,本文综述了氧化物(一元、二元、多元)稳定ZrO2、MZrO3化合物及Ln2Zr2O7化合物的研究情况。结果指出氧化物稳定ZrO2在热障涂层上的应用空间已十分有限,随着航空发动机技术的发展,化学式为A32 B24 O7焦绿石结构的陶瓷材料有望替代YSZ,根据声子导热理论和晶体化学原理,用稀土元素离子对A32 B24 O7型陶瓷材料进行掺杂进一步降低其热导率,将为热障涂层技术应用开辟广阔的空间。该机理对MZrO3同样适用。     

细水雾喷头喷射压力影响灭火性能的实验

为了研究细水雾喷头在不同喷射压力情况下针对油盘火的灭火效果,采用正庚烷为火灾燃料,在4.6m×3.3m×4m(长×宽×高)的空间内,针对同一型号的细水雾喷头在不同喷射压力下进行了灭火实验,在实验过程中采用热电偶树和气体分析仪对火焰温度及火场氧浓度进行了测量,得到了不同喷射压力下细水雾灭火的影响规律,为细水雾灭火设计、检验标准制定及细水雾灭火产品的开发提供了相应的实验依据.