高压质子交换膜水电解技术研究

介绍了国内外质子交换膜水电解技术的研究进展,讨论了阳极催化剂材料、膜厚度、电流密度对膜电极电化学性能的影响,利用高压水电解制氧测试平台分析了高压大功率质子交换膜水电解器的工作性能和长期运行稳定性的影响。结果表明,以Ir O2复合金属氧化物催化剂的膜电极,在80℃和1.0 A/cm2的条件下,电解单槽电压不大于1.75 V,水电解器氧气输出压力达到5 MPa,最大产氧量为3.6 Nm3/h,氧气纯度不小于99.5%,研制的水电解器具备在高压、大电流密度下稳定工作的能力。     

A Thermodynamic Approach to the Magnetospheric Complexity: The Role of Fluctuations

Recent studies evidenced that the magnetotail dynamics looks like the one of an avalanching system. This fact has been related with a near criticality dynamics and modelled by singular diffusion and transport equations. Here, we discuss some features of the Earth’s magnetotail dynamics using a thermodynamic approach. In detail we discuss the role played by fluctuations in singular diffusion and relaxation processes from a non-equilibrium thermodynamics point of view. Moreover, the emergence of non-Gaussian statistics is discussed in the framework of the thermodynamics of composite systems.     

CMH模型中部分参数对磁滞回线形状影响的研究

研究了Complete Moving Hysteresis模型计算公式中部分参数对磁滞回线形状的影响 ,发现饱和磁化强度Ms 和移动参数α对回线形状的影响并不显著 ,但参量γ的影响却是明显的 ,随着γ值的增加 ,回线的斜率增加 ,突变性增强     

空间开发中的国际合作机制问题

回顾国际空间合作历史及相关问题。以法国国家科学研究中心研究为例，对未来国际空间开发合作机制进行了实验性探讨，分析了俄、美两国空间开发中的不同主张及合作前景。     

战斗机滚转姿态快速性研究

介绍了战斗机中等幅度滚转姿态快速性的定义，应用欧拉法对19种飞机构形的滚转快速性进行了仿真计算．其结果与地面模拟战斗机攻击机动试验相比较，表明滚转姿态快速性与滚转模态时间常数、滚转操纵效能、副翼操纵速率和控制系统增益等飞行品质要求密切相关，飞行品质标准MIL—STD—1797没有完全涵盖中等幅度滚转姿态变化的要求。     

小展弦比飞机非线性气动特性风洞与飞行相关性研究

在较大迎角范围，如何由风洞试验数据预计全尺寸小展弦比飞机的非线性气动特性，并与飞行值相关，始终是国际航空界致力解决的重大问题，本项研究采用风洞试验与工程计算相结合的方法，对支架，洞壁、进气，喷流，雷诺数及静弹性等影响相关性的诸因素予以修正，并计及配平影响，从而比较准确地预计出全尺寸收音机的非线性气动特性，预计值与试飞值相比较结果验证了本项研究的可靠性和实用性。     

Who is who in Algol-land ? - Part II -

In part I (De Greve and Packet) we have investigated the occurrence of reversed phases of mass-transfer during Case A evolution in close binaries. If the initial period of a system is shorter than 1–2 days (Early Case A) the reversed phase starts before core hydrogen exhaustion of the gainer (part I). This type of evolution is characterized by at least two phases of slow mass-transfer.We have computed the evolution of four Early Case A systems with initial masses of the loser equal to 3 Mo and 5 Mo. These four systems start mass-exchange when Xc of the primary has decreased to 0.525 (75% of its initial value). They all experience two phases of slow mass-transfer.We find that both phases have about the same duration for all systems. The mass ratios are clearly distinct, being closer to unity during the first phase. In the Hertzsprung-Russell, mass-radius and mass-luminosity diagrams both components remain close to the main-sequence band during slow mass-transfer. Evolution as an Algol is ended when both components overflow their outer critical surface after a second reversal of the mass-transfer.Observed Algol systems evolving in Early Case A are scarce. A search thruogh the catalogue by Giuricin et al. gives us the following candidates: X Tri, SX Aur and V Pup. Based on their mass ratios, SX Aur can tentatively be assigned to the first phase of slow mass transfer and X Tri to the second phase. For V Pup (which is more massive) this choice can not be made with certainty.     

The transient highly excited solar flare plasma

Recent observations of the energetic particles produced in solar flares indicate that the production of electrons, with energies up to about 100 keV, is a fairly common feature of small flares. In those flares the acceleration of protons and other nuclei does not extend beyond about 1 MeV.The X-ray emission often exhibits two distinct components of which the first one is produced by non-thermal, the second by thermal electrons through bremsstrahlung collisions with the ambient ions. Along with these X rays, radio emission, in the microwave region, is observed. This radio emission is usually interpreted as due to gyrosynchrotron radiation from the same electrons.In this review a discussion is presented of the processes occurring in solar flares with special reference to the acceleration and radiation processes.     

The X-ray background 2–50 kev: A superposition of known sources,or evidence of a new component?

The contribution of the canonical Quasars to the XRB 2–50 keV is not likely to exceed 50%. Nay, consideration of X-ray selection effects results in a further reduction of the value of sensible estimators for the intensity ratio L_X/L_O; in addition, recent counts of radioloud and radio-quiet Quasars definitely limit the number of faint sources. A missing component with definite spectral properties should comprise a sizeable fraction of the XRB.