48GHz微带阵列天线设计

在5G高速发展的背景下,为实现机舱内部信息传输的无线化,设计了一款用于飞机设备舱内无线通信的毫米波微带阵列天线。结合串联馈电和并联馈电优点,采用串并联结合的方式对馈电网络进行设计。通过泰勒综合法实现阵元的同相位不等幅馈电,在保证高增益的情况下,有效地进行副瓣抑制。综合以上方法,设计出了一款中心频率为 48 GHz;在 47.3 ~48.7 GHz之间回波损耗小于-10 dB,工作带宽1.4 GHz;H 面上的半功率波束宽度小于 11°,副瓣抑制为-28 dB:E面上的半功率波束宽度小于 17°,副瓣抑制优于-21 dB 的4x8 微带天线阵,该阵列天线很好地实现了高增益/地旁瓣的特性。     

舰载机机舰电磁兼容性适配技术研究

机舰适配性是舰载飞机总体设计的核心内容之一。近年来,随着不同作战用途舰载机及舰载无人机的上舰服役,舰机总体单位对机舰电磁兼容适配越来越重视,随着多种舰载机编队协同作战,机舰平台频谱资源愈发紧张,机舰电磁兼容性问题越来越突出,机舰电磁兼容适配性的影响也愈发突出,频谱不兼容导致的问题严重影响舰载机的作战性能。尤其是以无线电测控链为主要通信方式的舰载无人机,飞机测控系统布置在母舰上,无论是电磁安全问题,还是电磁频谱兼容问题都将更加突出。主要闸述舰载机,尤其是舰载无人作战飞机上舰后,从舰载机机舰电磁兼容适配的主要需求为切人点,从机舰作为一体化装备的角度,阐明了机舰电磁兼容适配设计的诸多要素。依据如何更好地发挥作战能力的原则,对机舰电磁兼容适配设计做了较为系统的描述。     

Magnetic connectivity and solar energetic proton event intensity profiles at deka-MeV energy

We present an analysis of the time-intensity profiles of 25 solar energetic proton events at 18.2 MeV, modelled by fitting an analytical function form (a modified Weibull function) to the observed intensities. Additionally relying on previous work that characterized the magnetic connectivity between the event-related solar flare and the observer in these events with three angular parameters, we investigate the fit function parameters, the connectivity parameters, and the iron-to-carbon ratio of the events for dependencies and correlations. We find that the fit parameter controlling the basic shape of the profile (parameter a) is not clearly dependent on the connectivity parameters or the Fe/C ratio, suggesting that the profile shapes of neither well and weakly connected nor generally “impulsive” and “gradual” events differ systematically during the early stages of the event at 1 AU. In contrast, the time scaling of the fit function (parameter b) is at least moderately correlated with both the magnetic connectivity parameters and the Fe/C ratio, in that well-connected and iron-rich events are typically shorter in relative duration than weakly connected and nominal-abundance events; intensity rise times display a similar correlation with the connectivity parameters. We interpret the former result as following from the combined effect of various transport processes acting on the particles in interplanetary space, while the latter is essentially consistent with established knowledge regarding the observed dependence of the time-intensity profile shapes of solar energetic particle events on their magnetic connectivity and heavy ion abundances. The desirability of modelling the particle transport effects in detail and extending the analysis to cover higher energies is indicated.     

Catching spiral – S0 transition in groups. Insights from SPH simulations with chemo-photometric implementation

We are investigating the co-evolution of galaxies within groups combining multi-wavelength photometric and 2D kinematical observations. Here we focus on S0s showing star formation in ring/arm-like structures. We use smooth particle hydrodynamical simulations (SPH) with chemo-photometric implementation which provide dynamical and morphological information together with the spectral energy distribution (SED) at each evolutionary stage. As test cases, we simulate the evolution of two such S0s: NGC 1533 and NGC 3626.     

Galaxy evolution in groups. USGC U268 and USGC U376 in the Leo cloud

With the aim of investigating galaxy evolution in nearby galaxy groups, we analyzed the spectral energy distribution of 24 galaxies, members of two groups in the Leo cloud, USGC U268 and USGC U376. We estimated the ages and stellar masses of the galaxies by fitting their total apparent magnitudes from far-ultraviolet to near-infrared with population synthesis models. The comparison of the results for a subsample of galaxies with smooth particle hydrodynamic (SPH) simulations with chemo-photometric implementation, shows that in most cases the estimated stellar masses obtained with the two different approaches are in good agreement. The kinematical and dynamical analysis indicates that USGC U268 is in a pre-virial collapse phase while USGC U376 is likely in a more evolved phase towards virialization.     

Solar physics with the Square Kilometre Array

The Square Kilometre Array (SKA) will be the largest radio telescope ever built, aiming to provide collecting area larger than 1?km². The SKA will have two independent instruments, SKA-LOW comprising of dipoles organized as aperture arrays in Australia and SKA-MID comprising of dishes in South Africa. Currently the phase-1 of SKA, referred to as SKA1, is in its late design stage and construction is expected to start in 2020. Both SKA1-LOW (frequency range of 50–350?MHz) and SKA1-MID Bands 1, 2, and 5 (frequency ranges of 350–1050, 950–1760, and 4600–15,300?MHz, respectively) are important for solar observations. In this paper we present SKA’s unique capabilities in terms of spatial, spectral, and temporal resolution, as well as sensitivity and show that they have the potential to provide major new insights in solar physics topics of capital importance including (i) the structure and evolution of the solar corona, (ii) coronal heating, (iii) solar flare dynamics including particle acceleration and transport, (iv) the dynamics and structure of coronal mass ejections, and (v) the solar aspects of space weather. Observations of the Sun jointly with the new generation of ground-based and space-borne instruments promise unprecedented discoveries.     

Reverberation time lags in the high luminosity quasar PG 1247+267

Virial estimates of the black hole mass in the center of AGNs, derived from single-epoch observations of luminosity and emission line widths, are now available for several thousands of objects at all redshifts and luminosities, so that studies of the cosmological evolution of the AGN mass function are becoming possible. These estimates are based on the empirical luminosity-size relation measured through reverberation mapping at low redshifts and luminosities. For this reason the spectrophotometric monitoring of 4 luminous quasars was started in 2003, with the 1.8 m telescope of the Asiago Observatory. To measure the reverberation time lag we adopt a method, recently introduced by Zu et al. (2011), which takes advantage of the available statistical information on variability autocorrelation and makes simple assumptions on the continuum-emission line transfer function. We present the estimate of the broad line region size for the quasar PG 1247+267, which is the most luminous object with reverberation measures to date. Virial products computed for C iv and C iii] emission lines provide consistent results. A possible flattening of the size-luminosity relation for C iv at high luminosity is suggested.     

Orbital corrections by a single-input impulsive control applied along the geomagnetic field

This paper examines the possibility of regular orbital corrections for a satellite controlled by an impulsive force applied along the induction vector of the local geomagnetic field. The main purpose of the correcting considered in the paper is to eliminate the drift in secular variation of the relative orbital parameters over the orbital period. The obtained results are applied to the formation flying problem. The developed method is tested using numerical simulation.     

航天器复杂约束姿态机动的自主规划

 研究了星载设备经受动态环境的多种几何约束和动力学约束时,航天器姿态机动历程的星上规划方法。将完整姿态映射为三维姿态描述空间中的点,姿态路径的规划问题转化为中间节点的规划。随机搜索空间中的一组节点,在相邻节点间采用施加动力学约束的Euler转动姿态制导律,并考查Euler转动过程中的几何约束。用快速搜索随机树方法搜索到可行解,再利用姿态空间特性对路径加以优化。仿真显示算法能在大范围内快速得到可行解,优化措施有助缩短机动时间。离散化的节点规划保证了复杂约束情况下解的有效性,并具有概率完备性。     

不同金属基体上W-C:H 溅射薄膜的摩擦学性能

采用非平衡磁控溅射技术在40Cr、9Cr18、GCr15、TC4及LY12等5种金属基体上沉积了钨掺杂含氢类金刚石(W-C:H)薄膜。采用Raman光谱仪、扫描电子显微镜、纳米硬度计及纳米划痕仪分别测试了薄膜的微结构、厚度、硬度及附着力,采用球-盘摩擦试验机及光学轮廓仪分别在干摩擦和PFPE脂润滑条件下评价了5种金属材料基体上薄膜的摩擦磨损性能。薄膜性能测试结果显示,该厚度为1μm的薄膜具有典型的类金刚石结构,硬度与弹性模量分别为11.56和128.34 GPa,附着力为645 m N;摩擦试验结果显示,在干摩擦条件下几种金属基体表面W-C:H薄膜的摩擦因数和磨损率差别比较显著,而在脂润滑条件下基体材料的影响较小;与干摩擦条件相比,脂润滑条件下薄膜的磨损可减少60%~75%;在干摩擦与脂润滑条件下,9Cr18与40Cr基体上的W-C:H薄膜摩擦体系分别具有最小的磨损率1.71×10-7mm3/(N·m)及4.55×10-8mm3/(N·m)。