旋成体大迎角侧向力的控制方法计算研究

提出了运用充气气囊控制旋成体大迎角非对称分离涡的思路,并通过求解雷诺平均Navier-Stokes方程模拟了不同形状充气气囊作用下的流场,得到了充气气囊形状对旋成体侧向力的影响规律,计算结果表明充气气囊完全可以形成期望的流动干扰,为飞行器大迎角侧向力的控制探索了一条新的途径。     

Variation in the ionospheric propagating factor M(3000)F2 at Ouagadougou,Burkina Faso

We use hourly monthly median values of propagation factor M(3000)F2 data observed at Ouagadougou Ionospheric Observatory (geographic12.4°N, 1.5°W; 5.9^o dip), Burkina Faso (West Africa) during the years Januar1987–December1988 (average F10.7 < 130 × 10⁻²² W/m²/Hz, representative of low solar flux conditions) and for January 1989–December1990 (average F10.7 ? 130 × 10⁻²² W/m²/Hz, representative of high solar epoch) for magnetically quiet conditions to describe local time, seasonal and solar cycle variations of equatorial ionospheric propagation factor M(3000)F2 in the African region. We show that that seasonal trend between solar maximum and solar minimum curves display simple patterns for all seasons and exhibits reasonable disparity with root mean square error (RMSE) of about 0.31, 0.29 and 0.26 for December solstice, June solstice and equinox, respectively. Variability Σ defined by the percentage ratio of the absolute standard deviation to the mean indicates significant dissimilarity for the two solar flux levels. Solar maximum day (10–14 LT) and night (22–02 LT) values show considerable variations than the solar minimum day and night values. We compare our observations with those of the IRI 2007 to validate the prediction capacity of the empirical model. We find that the IRI model tends to underestimate and overestimate the observed values of M(3000)F2, in particular, during June solstice season. There are large discrepancies, mainly during high solar flux equinox and December solstice between dawn and local midnight. On the other hand, IRI provides a slightly better predictions for M(3000)F2 between 0900 and 1500 LT during equinox low and high solar activity and equinox high sunspot number. Our data are of great importance in the area of short-wave telecommunication and ionospheric modeling.     

Geomagnetic activity driven by solar wind turbulence

Within the framework of the solar wind—magnetosphere coupled system, intense perturbations in the solar wind, causing geomagnetic storms and substorms, have been widely studied by means of the so-called coupling parameters. However, remarkable variations in the geomagnetic field occur even in absence of such perturbations. In those conditions, solar wind MHD turbulence might have a role. Recent results have shown that solar wind turbulence can be described not only as a mixture of inward and outward stochastic Alfvénic fluctuations, but includes also advected structures, dominated by an excess of magnetic energy.     

太阳电池阵列模拟器计量测试方法研究

对太阳电池阵列模拟器(SAS)的设计原理和技术要求进行了分析,并根据分析结果对太阳电池阵列模拟器计量测试方法进行了研究。     

The effects of the solar magnetic polarity and the solar wind velocity on Bz-component of the interplanetary magnetic field

We have studied the effect of both solar magnetic polarity and the solar wind velocity on the Bz-component of the interplanetary magnetic field, IMFBz, for the minimum activity of the solar cycles 21, 22, 23 and 24. We made a statistical study of IMFBz in the first section which is considered as an extension of Lyatsky et al. (2003). They made a statistical study of IMFBz for two periods of minimum solar activity 22 and 23 related to 1985–1987 and 1995–1997 when the solar magnetic field had opposite polarity. Our results seem to be consistent with the results obtained by Lyatsky et al. (2003). We found that there is a dependence of IMFBz on the IMFBx and the solar magnetic polarity for the minimum periods of the selected four solar cycles. In addition, we found that there is a dependence of IMFBz on the solar wind velocity.     

基于循环平稳性的噪声调频干扰高分辨测向方法

根据噪声调频信号循环平稳特性分析,提出了基于阵列接收信号循环均值-空域处理的波达方向(DOA)估计算法。仿真结果表明:该算法的角度估计性能明显高于比幅比相单脉冲测角法,且在高信噪比环境中,该法的估计性能更好、运算量较小。     

Space observations of comets during solar flares: A possible explanation for comet brightness outbursts

Problems connected with mechanisms for comet brightness outbursts as well as for gamma-ray bursts remain open. Meantime, calculations show that irradiation of a certain class of comet nuclei, having high specific electric resistance, by intense fluxes of energetic protons and positively charged ions with kinetic energies more than 1 MeV/nucleon, ejected from the Sun during strong solar flares, can produce a macroscopic high-voltage electric double layer with positive charge in the subsurface zone of the nucleus, during irradiation times of the order of 10–100 h at heliocentric distances around 1–10 AU. The maximum electric energy accumulated in such layer will be restricted by the electric discharge potential of the layer material. For comet nuclei with typical radii of the order of 1–10 km the accumulated energy of such natural electric capacitor is comparable to the energy of large comet outbursts that are estimated on the basis of ground based optical observations. The impulse gamma and X-ray radiation together with optical burst from the comet nucleus during solar flares, anticipated due to high-voltage electric discharge, may serve as an indicator of realization of the processes above considered. Multi-wavelength observations of comets and pseudo-asteroids of cometary origin, having brightness correlation with solar activity, using ground based optical telescopes as well as space gamma and X-ray observatories, during strong solar flares, are very interesting for the physics of comets as well as for high energy astrophysics.     

大航向角误差情况下飞行中对准研究

为了解决飞行器在大航向角误差的情况下进行飞行中对准的难题,将一种线性大航向角误差模型应用于飞行器飞行中对准的过程.详细推导了线性大航向角误差模型,设计了飞行器在大航向角误差情况下进行飞行中对准的卡尔曼滤波模型,并进行了数字仿真.仿真结果表明,线性大航向角误差模型应用于飞行器飞行中对准,能够很好地解决飞行器在大航向角误差情况下进行对准的难点,并给出了适合于大航向角误差模型的机动方式.最后,提出了线性大航向角误差模型在工程应用中的几点建议     

最佳传力特性的偏置曲柄滑块机构解析法设计

本文根据偏置曲柄滑块机构的运动特性和传力特性所建立的函数关系，运用极值理论推导出给定条件下传力特性最佳的计算公式，大大方便了设计应用，值得推广。     

三叉杆式万向联轴器采用调心轴承时的运动分析

分析了三叉杆式万向联轴器采用调心轴承时输出转角和输入转角之间的关系式,并得出这种联轴器为准等角速传动万向联轴器的结论;讨论了轴偏转角大小对输出输入转角差值的影响,分析表明,这种联轴器中转角差值的变化周期是输入轴自转周期的3倍。