Evaluation of the influence of a measurable parameter error on precision of determining αΣ and Tg* by regression models

We present the regression models for determining the total excess air ratio α_Σ and gas temperature T _g ^* upstream of the high-pressure turbine formed on the basis of the engine parameter values that are regularly measured. The sensitivity of the regression models presented to the sensor and instrumentation precision is studied. The errors of measuring and calculating α_Σ and T _g ^* in different altitude-speed engine operation conditions are shown.     

Effects of RRA Treatments on Microstructures and Properties of a New High-strength Aluminum-Lithium Alloy-2A97

A new high strength 2A97 Al-Cu-Li-X alloy was subjected to triple-aging of retrogression and re-aging treatments (RRA). Transmission electron microscopy (TEM), differential scanning calorimetry (DSC), and tensile tests were used to investigate the effects of RRA treatment on the microstructures and properties. DSC test reveals the reversion temperature range of the strengthening δ' (Al3Li)phase. The results show that the microstructure consists of δ' (Al3Li) phase, T1 (Al2CuLi) phase and θ"/θ'(Al2Cu) phase for 2A97 alloy treated by a triple-aging ora retrogression and re-aging treatment in the following order: (1) at 165 ℃×30 min, (2) at 220 ℃ or 240 ℃×15 min, (3) at 165 ℃×24 h. The plastic deformation, incorporated into the treatment after secondary high temperature aging, promotes the T1 precipitation during final re-aging. The tensile properties of the alloy treated by the retrogression and re-aging treatment reach the peak level of alloy single-aged at 165 ℃ in T6 temper.     

RFI 用酚醛树脂体系的固化动力学和TTT 图

研制了适合树脂膜熔渗工艺(RFI)的酚醛树脂体系,采用动态DSC技术和固化度的测试,建立了改性树脂体系的固化动力学模型,研究了等温条件下固化度/温度/时间关系以及固化度/玻璃化转变温度关系,通过平板拉丝法研究树脂的凝胶过程,得出凝胶时间和温度之间的关系,回归得到凝胶时的固化度为αgel=53.33％,并以此计算出凝胶时的Tg,gel=48.64℃,在此基础上绘制了该体系的TTT图.     

Ion Acoustic Waves in the Heliosphere

Observations of ion acoustic waves in the solar wind during the first and second orbit of the Ulysses spacecraft are presented. The observations show variations of the wave activity with the heliolatitude and with the phase of the solar cycle. The interrelationships between the wave intensity and the electron heat flux and the ratio of electron to proton temperature, T _e/T _p, are examined. This revised version was published online in August 2006 with corrections to the Cover Date.     

Tailored analyses of 24 Galactic WN stars

The fundamental properties of 24 Galactic WN stars are determined from analyses of their optical, UV and IR spectra using sophisticated model atmosphere codes (Hillier, 1987, 1990). Terminal velocities, stellar luminosities, temperatures, mass loss rates and abundances of hydrogen, helium, carbon, nitrogen and oxygen are determined. Stellar parameters are derived using diagnostic lines and interstellar reddenings found from fitting theoretical continua to observed energy distributions.Our results confirm that the parameters of WN stars span a large range in temperature (T_*=30–90,000 K), luminosity (log L_*/L=4.8–5.9), mass loss (M=0.9–12×10^–5 M yr^–1) and terminal velocity (v =630–3300 km s^–1). Hydrogen abundances are determined, and found to be low in WNEw and WNEs stars (<15% by mass) and considerable in most WNL stars (1–50%). Metal abundances are also determined with the nitrogen content found to lie in the range N/He=1–5×10^–3 (by number) for all subtypes, and C/N 0.02 in broad agreement with the predictions of Maeder (1991). Enhanced O/N and O/C is found for HD 104994 (WN3p) suggesting a peculiar evolutionary history. Our results suggest that single WNL+abs stars may represent an evolutionary stage immediately after the Of phase. Since some WNE stars exist with non-negligible hydrogen contents (e.g. WR136) evolution may proceed directly from WNL+abs to WNE in some cases, circumventing the luminous blue variable (LBV) or red supergiant (RSG) stage.     

In situ Wave Phenomena Associated with Magnetic Clouds and Other Ejecta

We present Ulysses Unified Radio and Plasma Wave (URAP) observations of ion-acoustic waves associated with magnetic clouds and ejecta. The peak intensities of these waves, which usually occur inside CMEs when T _e/T _i≫1, are not correlated with heliocentric distance or electron to ion temperature ratio inside the CMEs. This revised version was published online in August 2006 with corrections to the Cover Date.     

T800/5228A层合板Ⅰ型断裂韧性优化

冷场发射扫描电镜表明,固化5228A/PAEK共混体系发生了反应诱导相分了海岛-双连续-相反转的演化过程;DMA试验表明,PAEK的引入对5228A基体树脂T会改变原有树脂体系的使用温度;T800/5228A经韧化后,在层间内形成了典型的相反转结现出波纹状,明显区别于原有的光滑平直裂纹路径,Ⅰ型层间断裂韧度(GIC)大幅度提高.     

Dynamical theory of the solar wind

This paper is a review of the basic theoretical dynamical properties of an atmosphere with an extended temperature strongly bound by gravity. The review begins with the historical developments leading up to the realization that the only dynamical equilibrium of an atmosphere with extended temperature is supersonic expansion. It is shown that sufficient conditions for supersonic expansion are T(r) declining asymptotically less rapidly than 1/r, or the density at the base of the corona being less than N _b given by (40) if no energy is available except through thermal conductivity, or the temperature falling within the limits given by (18) if T N ^-1 throughout the corona. Less extended temperatures lead to equilibria which are subsonic or static. The hypothetical case of a corona with no energy supply other than thermal conduction from its base is considered at some length because the equations may be solved by analytical methods and illustrate the transition from subsonic to supersonic equilibrium as the temperature becomes more extended. Comparison with the actual corona shows that the solar corona is actively heated for some distance into space by wave dissipation.The dynamical stability of the expanding atmosphere is demonstrated, and in a later section the radial propagation of acoustic and Alfvén waves through the atmosphere and wind is worked out. The calculations show that the magnetometer will probably detect waves more easily than the plasma instrument, but that both are needed to determine the mode and direction of the wave. An observer in the wind at the orbit of Earth can listen to disturbances generated in the corona near the sun and in turbulent regions in interplanetary space.The possibility that the solar corona is composed of small-scale filaments near the sun is considered. It is shown that such filamentary structure would not be seen at the orbit of Earth. It is pointed out that the expansion of a non-filamentary corona seems to lead to too high a calculated wind density at the orbit of Earth to agree with the present observations, unless T(r) is constant or increases with r. A filamentary corona, on the other hand, would give the observed wind density for declining T(r).It is shown that viscosity plays no important role in the expansion of an atmosphere either with or without a weak magnetic field. The termination of the solar wind, presumably between 10–10³ AU, is discussed briefly. The interesting development here is the interplanetary L recently observed, which may come from the interstellar neutral hydrogen drifting into the outer regions of the solar wind.Theory is at the present time concerned with the general dynamical principles which pertain to the expansion equilibrium of an atmosphere. It is to be expected that the rapid progress of direct observations of the corona and wind will soon permit more detailed studies to be carried out. It is important that the distinction between detailed empirical models and models intended to illustrate general principles be kept clearly in mind at all times.This work was supported by the National Aeronautics and Space Administration under Grant NASA-NsG-96-60.     

八水氢氧化钡相变材料的强化传热实验

采用差示扫描量热法(DSC)对八水氢氧化钡相变材料进行热物性分析,总结出一种针对结晶水合盐相变温度与潜热准确可靠的测量方法.通过扫描电子显微镜(SEM)获得相变材料与金属容器截面腐蚀情况的图像,证明八水氢氧化钡与紫铜有优良的相容性.分别对含/未含泡沫铜的固液相变蓄热体进行实验研究,结果表明:泡沫铜填充使相变材料在固相区内熔化时间减少了26%,增强了相变材料的传热效果,而且将八水氢氧化钡过冷度降低了50%.      

Electron density and temperature,as measured by the mutual impedance experiment on board GEOS-1

The mutual impedance experiment on GEOS-1 provides an original diagnostic of the thermal electron population. The electron density N _e, and temperature T _e, are derived from the plasma frequency and Debye length, the values of which determine the shape of the frequency dependent mutual impedance curves. The existing limits of the method are pointed out. They may be instrumental or arise from a lack of theoretical development, for instance when the steady magnetic field or the drift velocity of the plasma cannot be neglected. Nevertheless, first geophysical results have been derived, using measurements obtained on the dayside of the equatorial magnetosphere where most of the data enter within the above limits. In particular, we have drawn a map of the dayside magnetosphere, in terms of densities, Debye lengths, temperatures, at geocentric distances of 4 to 7 Earth radii. The conventional shape of the plasmasphere is recognized, but the temperatures obtained are lower than expected (2 eV at apogee, outside the plasmasphere). The influence of the magnetic activity on apogee measurements is reported: N _e values and A _m indices are shown to be correlated, but it is not the case for T _e and A _m. Finally, detailed T _e and N _e profiles are shown, and the presence of a plasmapause boundary is discussed.     

Assessment of gas temperature fluctuations in the GTE combustion chamber exit section at generalizing experimental data on fuel combustion efficiency

It is suggested that gas composition at every point of the combustion chamber exit section be characterized by the temperature values T _i (“ideal” temperature) corresponding to the local values of the air-to-fuel coefficient α _i under complete fuel combustion (ν _comb ≈ 1). It is assumed that the values of T _i are distributed over the exit section area (gas mass) linearly and the values of T _imax and T _imin can be determined by the experimental data on the gas temperature fields in the combustion chambers. The distribution of temperatures T _i is used when it is necessary to generalize the experimental data on fuel combustion efficiency in GTE combustion chambers.     

Competing effects of surface catalysis and ablation in hypersonic reentry aerothermodynamic environment

Under hypersonic flow conditions, the complicated gas-graphene interactions including surface catalysis and surface ablation would occur concurrently and intervene together with the thermodynamic response induced by spacecraft reentry. In this work, the competing effects of surface heterogeneous catalytic recombination and ablation characteristics at elevated temperatures are investigated using the Reactive Molecular Dynamics (RMD) simulation method. A Gas-Surface Interaction (GSI) model is established to simulate the collisions of hyper-enthalpy atomic oxygen on graphene films in the temperature range of 500–2500 K. A critical temperature T_c around 900 K is identified to distinguish the graphene responses into two parts: at T < T_c, the heterogeneous surface catalysis dominates, while the surface ablation plays a leading role at T > T_c. Contradicting to the traditional Arrhenius expression that the recombination coefficient increases with the increase of surface temperature, the value is found to be relatively uniform at T < T_c but declines sharply as the surface temperature increases further due to the competing ablation effect. The occurrence of surface ablation decreases the amounts of active sites on the graphene surface for oxygen adsorption, leading to reduced recombination coefficient from both Langmuir-Hinshelwood (L-H) and Eley-Rideal (E-R) mechanisms. It suggests that the traditional Computational Fluid Dynamics (CFD) simulation method, which relies on the Arrhenius-type catalysis model, would result in large discrepancies in predicting aerodynamic heat for carbon-based materials during reentry into strong aerodynamic thermal environment.     

The stellar content of the Orion OB1 association

We present a photometric investigation, using the VBLUW system, of the stellar content of Orion OB1. Physical parameters (logg, logT _eff) for the stars are derived with the aid of model atmospheres. From these, visual extinctions, absolute magnitudes and distance moduli are derived. The distance moduli are used to determine membership for the stars in each of the subgroups and distances to the subgroups are calculated. The ages of the subgroups are derived through isochrone fitting and the IMF is derived for each subgroup. The energy deposited into the ISM through stellar winds and supernovae is calculated and compared to observed large scale features in the ISM around Orion OB1.     

The near-Earth plasma sheet: An AMPTE/IRM perspective

During the last five years, statistical studies using plasma measurements made by the AMPTE/IRM satellite have lead to a better understanding of the structure and dynamics of the near-Earth plasma sheet between about 10 and 20R _E. The most notable new findings are: (1) the adiabatic non-isentropic behavior of the tail plasma during quiet times; (2) the strong non-adiabatic heating of ions and electrons during substorms and the strong coupling of the ion and electron temperature withT _i/T_i7; and (3) the high-speed flow bursts which carry most of the tail plasma transport. Moreover, it became clear that it is the central plasma sheet, and not the plasma sheet boundary layer, which is most affected by substorm activity.     

Phase Transformation and Microstructure of Ti50Ni48-xFe2Ndx Shape Memory Alloys

The influences of rare earth element Nd on the phase transformation and the microstructure of Ti₅₀Ni_48−xFe₂Nd_x shape memory alloys are investigated by means of electrical resistivity, optical microscopy, electron probe microanalyzer, and X-ray diffraction. The results show that TiNiFe alloys with different Nd contents exhibit two-step martensitic transformation. The start temperature of martensitic transformation increases sharply from 212 K to 267 K when 0.1 at.% Nd is added in, and then decreases gradually if Nd content further increases. The microstructure of TiNiFeNd quaternary alloys consists of TiNi matrix, Ti₂Ni second phase, and Nd₃Ni intermetallic compound. The spherical Nd₃Ni precipitate-particles evenly disperse in the matrix.     

Electron-Ion Temperature Equilibration in Collisionless Shocks: The Supernova Remnant-Solar Wind Connection

Collisionless shocks are loosely defined as shocks where the transition between pre-and post-shock states happens on a length scale much shorter than the collisional mean free path. In the absence of collision to enforce thermal equilibrium post-shock, electrons and ions need not have the same temperatures. While the acceleration of electrons for injection into shock acceleration processes to produce cosmic rays has received considerable attention, the related problem of the shock heating of quasi-thermal electrons has been relatively neglected. In this paper we review the state of our knowledge of electron heating in astrophysical shocks, mainly associated with supernova remnants (SNRs), shocks in the solar wind associated with the terrestrial and Saturnian bowshocks, and galaxy cluster shocks. The solar wind and SNR samples indicate that the ratio of electron temperature, (T _e ) to ion temperature (T _p ) declining with increasing shock speed or Alfvén Mach number. We discuss the extent to which such behavior can be understood on the basis of waves generated by cosmic rays in a shock precursor, which then subsequently damp by heating electrons, and speculate that a similar explanation may work for both solar wind and SNR shocks.     

热轧对Ti50Ni50-xAlx(x=1,2,4)形状记忆合金微观组织、相变和力学性能的影响

形状记忆合金的相变和力学性能受机械加工过程影响明显.在850℃下将Ti50Ni50-xAIx(x=1,2,4)形状记忆合金轧制成为板材.采用扫描电镜、透射电镜和X射线衍射对合金的微观结构研究表明:合金由NiTi相和Ti2Ni相组成,Al元素在Ti2Ni相中的固溶度比在TiNi相中高.差示扫描量热分析和电阻-温度测试表明...     

Gain self-scheduled H_∞ control for morphing aircraft in the wing transition process based on an LPV model

This article investigates gain self-scheduled H 1 robust control system design for a tailless fold- ing-wing morphing aircraft in the wing shape varying process. During the wing morphing phase, the aircraft’s dynamic response will be governed by time-varying aerodynamic forces and moments. Nonlinear dynamic equations of the morphing aircraft are linearized by using Jacobian linearization approach, and a linear parameter varying (LPV) model of the morphing aircraft in wing folding is obtained. A multi-loop controller for the morphing aircraft is formulated to guarantee stability for the wing shape transition process. The proposed controller uses a set of inner-loop gains to provide stability using classical techniques, whereas a gain self-scheduled H 1 outer-loop controller is devised to guarantee a specific level of robust stability and performance for the time-varying dynamics. The closed-loop simulations show that speed and altitude vary slightly during the whole wing folding process, and they converge rapidly after the process ends. This proves that the gain self-scheduled H 1 robust controller can guarantee a satisfactory dynamic performance for the morphing aircraft during the whole wing shape transition process. Finally, the flight control system’s robustness for the wing folding process is verified according to uncertainties of the aerodynamic parameters in the nonlinear model.     

超洁净环境中三维非晶态凝固研究

采用超洁净环境对 Zr₄₁ Ti₁₄ Ni₁₀Cu_12.5 Be_22.5 合金进行电弧熔炼,在 1 0 0～ 1 50 K/s的慢速冷却条件下,成功地制备出厚度大于 1 0 mm的非晶合金。这是一种在超洁净环境中的部分无容器凝固,可以获得较大过冷度。随着熔炼过程中氧含量的增多,由于合金表面被氧化,氧化物作为异质晶核强烈促使液态合金结晶。利用红外测温方法快速检测了合金在凝固过程中非晶的形成。通过分析润湿角因子 f(θ)对合金形核与结晶过程的影响,获得了非晶态凝固所需临界冷却速率 Rc 与润湿角θ之间的关系。     

纤维素甘油醚硝酸酯粘合剂及其推进剂的力学性能

利用X-ray衍射、拉伸实验和动态力学性能DMA实验研究了纤维素甘油醚硝酸酯(NGEC)的结晶度、NGEC及其推进剂的力学性能和动态力学性能,借助扫描电镜观察了NGEC基改性双基推进剂的断裂形貌,并通过流动性实验探索了NGEC全部与部分取代NC的改性双基推进剂的热加工工艺性能。结果表明:与NC相比,NGEC的结晶度和力学强度略低、延伸率较高、玻璃化转变温度低且转变温度范围宽;加入NGEC,可降低高固体含量改性双基推进剂的脱湿现象,有利于提高其力学性能;粘合剂体系中NGEC的含量对其改性双基推进剂的玻璃化转变的α松弛影响较大,随着NGEC含量的增加α松弛温度明显降低,而对β松弛的影响较小;与NC相比,NGEC的加入降低了改性双基推进剂的流动性实验出药压力,提高了出药速度,具有良好的热塑性及热加工安全性。