NONLINEAR DYNAMIC INVERSION CONTROL WITH ADAPTIVE COMPENSATION FOR FLIGHT CONTROL SYSTEM

ＮＯＮＬＩＮＥＡＲＤＹＮＡＭＩＣＩＮＶＥＲＳＩＯＮＣＯＮＴＲＯＬＷＩＴＨＡＤＡＰＴＩＶＥＣＯＭＰＥＮＳＡＴＩＯＮＦＯＲＦＬＩＧＨＴＣＯＮＴＲＯＬＳＹＳＴＥＭＸｕＪｕｎ，ＺｈａｎｇＭｉｎｇｌｉａｎ，ＬｉＹｏｕｌｉａｎｇ（ＤｅｐａｒｔｍｅｎｔｏｆＡｕｔｏ...     

NUMERICAL STUDY OF TOPOLOGICAL STRUCTURE OF 3-D TRANSONIC VISCOUS FLOW FIELD (TVFF) INSIDE TURBINE CASCADE

ＮＵＭＥＲＩＣＡＬＳＴＵＤＹＯＦＴＯＰＯＬＯＧＩＣＡＬＳＴＲＵＣＴＵＲＥＯＦ３ＤＴＲＡＮＳＯＮＩＣＶＩＳＣＯＵＳＦＬＯＷＦＩＥＬＤ（ＴＶＦＦ）ＩＮＳＩＤＥＴＵＲＢＩＮＥＣＡＳＣＡＤＥＧｕｏＹａｎｈｕ，ＳｈｅｎＭｅｎｇｙｕ，ＷａｎｇＢａｏｇｕｏ（Ｄｅ...     

STUDY ON ROTOR HEAD VIBRATION ABSORBER OF HELICOPTER

ＳＴＵＤＹＯＮＲＯＴＯＲＨＥＡＤＶＩＢＲＡＴＩＯＮＡＢＳＯＲＢＥＲＯＦＨＥＬＩＣＯＰＴＥＲＧｕＺｈｏｎｇｑｕａｎ；ＰｅｎｇＦｕｊｕｎ；ＭａＫｏｕｇｅｎ（ＲｅｓｅａｒｃｈＩｎｓｔｉｔｕｉｅｏｆＶｉｂｒａｔｉｏｎＥｎｇ，ＮａｎｊｉｎｇＵｎｉｖｅｒｓｉｔｙ...     

THE PREDICTIONS OF CONVECTIVE HEAT TRANSFER ON TURBINE BLADE AIRFOIL BY USING LOW－REYNOLDS NUMBER TURBULENCE MODEL

ＴＨＥＰＲＥＤＩＣＴＩＯＮＳＯＦＣＯＮＶＥＣＴＩＶＥＨＥＡＴＴＲＡＮＳＦＥＲＯＮＴＵＲＢＩＮＥＢＬＡＤＥＡＩＲＦＯＩＬＢＹＵＳＩＮＧＬＯＷ－ＲＥＹＮＯＬＤＳＮＵＭＢＥＲＴＵＲＢＵＬＥＮＣＥＭＯＤＥＬＴＨＥＰＲＥＤＩＣＴＩＯＮＳＯＦＣＯＮＶＥＣＴＩＶＥ...     

SOFTWARE SERVO COURSE(ATTITUDE) SYSTEMS

ＳＯＦＴＷＡＲＥＳＥＲＶＯＣＯＵＲＳＥ（ＡＴＴＩＴＵＤＥ）ＳＹＳＴＥＭＳＺｈａｎｇＸｕｅｆｕ（ＨｕｎａｎＲａｄｉｏａｎｄＴＶＵｎｉｖｅｒｓｉｔｙ，Ｃｈａｎｇｓｈａ，Ｈｕｎａｎ，Ｃｈｉｎａ，４１０００４）ＳＯＦＴＷＡＲＥＳＥＲＶＯＣＯＵＲＳＥ（ＡＴＴＩ...     

HELICOPTER VIBRATION REDUCTION TECHNIQUE WITH HARMONIC ACTIVE CONTROL

ＨＥＬＩＣＯＰＴＥＲＶＩＢＲＡＴＩＯＮＲＥＤＵＣＴＩＯＮＴＥＣＨＮＩＱＵＥＷＩＴＨＨＡＲＭＯＮＩＣＡＣＴＩＶＥＣＯＮＴＲＯＬＹａｎｇＹｉｄｏｎｇ；ＹｕａｎＳｕｏｚｋｏｎｇ；ＹｕａｎＷｅｉｄｏｎｇ（Ｄｅｐｔ．ｏｆＡｕｔｏｍａｔｉｃＣｏｎｔｒｏｌ，Ｎａｎ...     

PARALLEL COMPUTATION OF SUPER-SONIC BLUNT BODY VISCOUS FLOWFIELDS IN PVM

ＰＡＲＡＬＬＥＬＣＯＭＰＵＴＡＴＩＯＮＯＦＳＵＰＥＲ┐ＳＯＮＩＣＢＬＵＮＴＢＯＤＹＶＩＳＣＯＵＳＦＬＯＷＦＩＥＬＤＳＩＮＰＶＭＹａｎｇＸｉａｏｈｕｉ，ＷａｎｇＺｈｅｎｇｈｕａ，ＷａｎｇＣｈｅｎｇｙａｏ（Ｄｅｐｔ．１，ＮａｔｉｏｎａｌＵｎｉｖｅｒｓｉｔ...     

ITERATIVE COMPUTATION METHOD FOR NONLINEAR FORCED VIBRATION EQUATION ON HELICOPTER MAIN ROTOR LOAD

ＩＴＥＲＡＴＩＶＥＣＯＭＰＵＴＡＴＩＯＮＭＥＴＨＯＤＦＯＲＮＯＮＬＩＮＥＡＲＦＯＲＣＥＤＶＩＢＲＡＴＩＯＮＥＱＵＡＴＩＯＮＯＮＨＥＬＩＣＯＰＴＥＲＭＡＩＮＲＯＴＯＲＬＯＡＤＬｉｕＸｉａｎｇｊｉａｎ；ＳｈｅｎＸｉｎｋａｎｇ；ＸｕｅＺｈｅｎｇｚｈｏｎｇ（...     

高阶各向异性k－ε模型及在直通道湍流流场中的数值研究

ＡＨＩＧＨ－ＯＲＤＥＲＡＮＩＳＯＴＲＯＰＩＣＫ－εＭＯＤＥＬＡＮＤＩＴＳＮＵＭＥＲＩＣＡＬＩＮＶＥＳＴＩＧＡＴＩＯＮＩＮＴＷＯＤＩＭＥＮＳＩＯＮＡＬＴＵＲＢＵＬＥＮＴＦＬＯＷＦＩＥＬＤＳＬｉｕＺｈｅｎｇｘｉａｎ，ＳｏｎｇＢａｏｊｕｎ，ＧｕＣｈｕａｎｇ...     

ANALYTICAL－GENERALIZED VARIATIONAL METHOD ABOUT SOLUTION OF SIF AND CONSERVATIVE INTEGRAL FOR DELAMINATlONS OF LAMINATE BEAM

ＡＮＡＬＹＴＩＣＡＬ－ＧＥＮＥＲＡＬＩＺＥＤＶＡＲＩＡＴＩＯＮＡＬＭＥＴＨＯＤＡＢＯＵＴＳＯＬＵＴＩＯＮＯＦＳＩＦＡＮＤＣＯＮＳＥＲＶＡＴＩＶＥＩＮＴＥＧＲＡＬＦＯＲＤＥＬＡＭＩＮＡＴｌＯＮＳＯＦＬＡＭＩＮＡＴＥＢＥＡＭＡＮＡＬＹＴＩＣＡＬ－ＧＥＮＥ...     

ALCATEL DVOR4000边带相位调整方法改进

对ALCATELDVOR4000型全向信标的边带相位调整方法进行了分析、推理，并结合实践提出了较好的调整方案。     

An Inverted VOR of Small Aperture

A new type of omnirange very-high-frequency omnidirectional radio (VOR), intended to be compatible with existing receivers, is described. It is ``inverted' in the sense that reference phase is transmitted by AM, as in the Doppler VOR (DVOR). Variable phase is radiated as a rotating square-wave FM field, the radiating elements being concentric loop antennas with circumferences equal to integer numbers of wave-lengths. Each loop radiates one term in the Fourier expansion of the variable phase field.     

Abundances of Deuterium and Helium-3 in the Protosolar Cloud

The mass spectrometric determinations of the isotopic composition of helium in the solar wind obtained from (1) the Apollo Solar Wind Composition (SWC) experiment, (2) the Ion Composition Instrument (ICI) on the International Sun Earth Explorer 3 (ISEE-3), and (3) the Solar Wind Composition Spectrometer (SWICS) on Ulysses are reviewed and discussed, including new data given by Gloeckler and Geiss (1998). Averages of the 3He/4He ratio in the slow wind and in fast streams are given. Taking account of separation and fractionation processes in the corona and chromosphere, 3He/4He = (3.8 ± 0.5) × 10-4 is derived as the best estimate for the present-day Outer Convective Zone (OCZ) of the sun. After corrections of this ratio for secular changes caused by diffusion, mixing and 3He production by incomplete H-burning (Vauclair, 1998), we obtain (D + 3He)/H = (3.6±0.5) × 10-5 for the Protosolar Cloud (PSC). Adopting 3He/H = (1.5±0.2) × 10-5 for the PSC, as is indicated from the 3He/4He ratio in the planetary gas component of meteorites and in Jupiter (Mahaffy et al., 1998), we obtain (D/H)protosolar = (2.1 ± 0.5) × 10-5. Galactic evolution studies (Tosi, 1998) show that the measured D and 3He abundances in the Protosolar Cloud and the Local Interstellar Cloud (Linsky, 1998; Gloeckler and Geiss, 1998), lead to (D/H)primordial = (2 - 5) × 10-5. This range corresponds to a universal baryon/photon ratio of (6.0 ± 0.8) × 10-10, and to b = 0.075 ± 0.015.     

Measurement of the Abundance of Helium-3 in the Sun and in the Local Interstellar Cloud with SWICS on Ulysses

The abundance of 3He in the present day local interstellar cloud (LIC) and in the sun has important implications for the study of galactic evolution and for estimating the production of light nuclei in the early universe. Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is used to measure the isotopic ratio of helium (3He/4He = ) both in the solar wind and the local interstellar cloud. For the solar wind, the unique high-latitude orbit of Ulysses allows us to study this ratio in the slow and highly dynamic wind in the ecliptic plane as well as the steady high-latitude wind of the polar coronal holes. The 3He+/4He+ ratio in the local cloud is derived from the isotopic ratio of pickup helium measured in the high-speed solar wind. In the LIC the ratio is found to be (2.48 _-0.62 ^+0.68 ) × 10^-4 with the 1- uncertainty resulting almost entirely from statistical error. In the solar wind, is determined with great statistical accuracy but shows systematic differences between fast and slow solar wind streams. The slow wind ratio is variable. Its weighted average value (4.08 ± 0.25) × 10-4 is, within uncertainties, in agreement with the Apollo SWC results. The high wind ratio is less variable but smaller. The average in the fast wind is (3.3 ± 0.3) × 10-4.     

三级数据的遥测交互软件架构设计及实现

针对遥测交互分系统实时处理数据量大、数据种类多样、数据收发模式灵活、技术状态变换频繁、软件维护要求高的问题,提出了一种数据池—数据表—数据通道的三级数据交互软件架构,该架构对交互分系统中所有数据进行高度抽象,采用通用化的处理过程,可以很好地适应各种需求。目前,基于该架构的遥测数据交互软件已在国产麒麟系统下实现,通过快捷、可视化的配置及灵活的人机交互,可以快速实现任务状态转换,能够满足各种航天测量任务的需求。这表明,该架构是一种理想、高效的数据交互软件通用解决方案,可推广到雷达、光学等其他测量设备。     

Adaptive processing at the subarray level

This paper describes a class of partially adaptive arrays with adaptive processing applied to the outputs of steered subarrays. The problem is to detect a signal or estimate its direction of arrival in the presence of jammers. The advantage of applying adaptive processing to subarrays is that it requires much less CPU time than the corresponding fully adaptive processing. The subarray processing equations for the two kinds of problem are described. In this paper, we compare partially adaptive processing performance with fully adaptive processing performance in the case of the following antenna and signal sources:

• •- array with regularly spaced sensors ;
• •- between 20 and 100 elements ;
• •- between 3 and 20 subarrays ;
• •- a single jammer ;
• •- desired signal from the antenna zenith.

We suggest a method for determining the optimal subarray configurations in this case. An example is given to show that the performance of an antenna with five subarrays is comparable to that of a fully adaptive thirty-element array for eliminating a single jammer with a target at the zenith.     

New Experimental Data and What It Tells Us About the Sources and Acceleration of Cosmic Rays

This paper summarizes new data in several fields of astronomy that relate to the origin and acceleration of cosmic rays in our galaxy and similar nearby galaxies. Data from radio astronomy shows that supernova remnants, both in our galaxy and neighboring galaxies, appear to be the sources of most of the accelerated electrons observed in these galaxies. -ray measurements also reveal several strong sources associated with supernova remnants in our galaxy. These sources have -ray spectra that are suggestive of the acceleration of cosmic-ray nuclei. Cosmic-ray observations from the Voyager and Ulysses spacecraft suggest a source composition that is very similar to the solar composition but with distinctive differences in the ⁴He, ¹²C,¹⁴ N and ²²Ne abundances that are the imprint of giant W-R star nucleosynthesis. Injection effects which depend on the first ionization potential (FIP) of the elements involved are also observed, in a manner similar to the fractionization observed between the solar photosphere and corona and also analogous to the preferential acceleration observed for high FIP elements at the heliospheric solar wind termination shock. Most of the ⁵⁹Ni produced in the nucleosynthesis of Fe peak nuclei just prior to a SN explosion appears to have decayed to ⁵⁹Co before the cosmic rays have been accelerated, suggesting that the⁵⁹ Ni is accelerated at least 10⁵ yr after it is produced. The decay of certain K capture isotopes produced during cosmic-ray propagation has also been observed for the first time. These measurements suggest that re-acceleration after an initial principal acceleration cannot be large. The high energy spectral indices of cosmic-ray nuclei show a significant charge dependent trend with the index of hydrogen being -2.76 and that of Fe -2.61. The escape length dependence of cosmic rays from our galaxy can now be measured up to ~300 GeV nucl^-1 using the Fe sec/Fe ratio. This escape length is P ^-0.05 above 10 GeV nucl^-1 leading to a typical source spectral index of (2.70±0.10) -0.50 = -2.20 for nuclei. This is similar to the source index of -2.3 inferred for electrons within the errors of ±0.1 in the index for both components. Spacecraft measurements in the outer heliosphere suggest that the local cosmic-ray energy density is ~2eV cm^-3 – larger than previously assumed. Gamma-ray measurements of electron bremsstrahlung below 50 MeV from the Comptel experiment on CGRO show that fully 20–30% of this energy is in electrons, several times that previously assumed. New estimates of the amount of matter traversed by cosmic rays using measurements of the B/C ratio are also higher than earlier estimates – this value is now ~10 g cm^-2 at 1 GeV nucl^-1. Thus altogether cosmic rays are energetically a more important component of our galaxy than previously assumed. This has implications both for the types of sources that are capable of accelerating cosmic rays and also for the role that cosmic rays may play in ionizing the diffuse interstellar medium.     

Experimental Detection of Anomalous Mode-C Reports Using Radar Data

A new methodology to scan automated radar terminal system (ARTS-III) data for aircraft tracks exhibiting probable mode-C encoder/transponder faults is described. The tracks of more than 8000 climbing or descending aircraft, recorded at the Seattle-Tacoma terminal area, were analyzed using this method. Based on this sample, the probability of the previously recognized "stuck C-bit" error is estimated to be 0.44 percent (0.31-0.61 percent, 95 percent confidence). In addition, a new, more subtle error, here termed the "deficient response," was discovered which is estimated to occur with a probability of 0.77 percent (0.59-0.98 percent, 95 percent confidence). Subsequent tests found this new error to have much less impact on traffic alert and collision avoidance system (TCAS) performance than does the stuck C-bit error.     

An IR,optical and X-ray study of the two state behaviour of GX 339-4

We review results of correlated IR, optical and X-ray observations of GX 339-4 made from March 1981 through May 1984. In the soft X-ray state, the object does not show outstanding optical and X-ray variability. Night-to-night smooth optical variations of 0.3 magnitudes were however present during one observing run. In contrast, the hard X-ray state is characterised by strong erratic optical and X-ray fluctuations on time scales from 20 milliseconds to seconds, as well as 7 to 20 second quasi-periodic oscillations. The optical counterpart appears much redder in the IR during the hard state. Particular attention is drawn to the hard to soft X-ray transition which occured in June 1981. The shape of the IR to X-ray energy distribution is discussed. The unusual features of this black hole candidate are examined in the framework of the current theories of accretion.Based partly on observations obtained at the European Southern Observatory, La Silla, Chile.     

The Low Metallicity Tail of the Halo Metallicity Distribution Function

Ongoing spectroscopy and photometry of stars selected in the HK objective-prism/interference-filter survey of Beers and colleagues has resulted in the identification of many hundreds of additional stars in the halo (and possibly the thick disk) of the Galaxy with abundances [Fe/H] -2.0. A new calibration of the technique for estimation of metal abundance based on a CaII K index as a function of broadband B - V color is applied to obtain metallicities for stars observed with the SSO 2.3m and INT 2.5m telescopes. This new data is combined with other samples of extremely metal-deficient stars (Ryan and Norris, 1991a; Beers et al., 1992; Carney et al., 1994) to form a large database of objects of low metallicity. The combined sample is examined and compared with expectations derived from a Simple Model of Galactic chemical evolution. There appears to be a statistically-significant deficit of stars more metal-weak than [Fe/H] = -3.0. An abundance of [Fe/H] -4.0 can be taken as the low-metallicity limit for presently-observable stars in the Galaxy.