超声爬波无损检测方法的研究

本文介绍了超声无损检测中一种具有较好应用前景的波型──超声爬波。试验研究了爬波检测时缺陷定位、定性评定的方法，并给出了主要结论。     

低纬地磁Z分量的半年变化

利用武汉、广州、泉州和琼中等4个低纬地磁站连续多年的地磁资料，计算了各月5个磁静日Z分量日均值与中午1100---1300时段平均值之差(Dz)，对每年12个Dz采用多元回归分析方法，得到各年的半年变化幅度和相位．结果表明：4个站的Dz每年都有半年变化现象；半年变化幅度与太阳活动有关，一般来说，太阳活动高年Dz半年变化幅度明显大于太阳活动低年；太阳活动本身的半年变化，对Dz半年变化幅度有显著的调制作用；Dz半年变化的相位在3—4月(或9—10月)，即极大值出现在分季；低纬地区地磁Z分量存在显著的半年变化，能够反映赤道电急流也有明显的半年变化，这再一次证明，赤道电急流幅度的半年变化，通过“喷泉效应”使得电离层，f0F2产生半年变化，其是产生，f0F2半年变化的一个主要因素．     

Spectra and time variability of black-hole binaries in the low/hard state

We propose a jet model for the low/hard state of galactic black-hole X-ray sources which explains the energy spectra from radio to X-rays and a number of timing properties in the X-ray domain such as the time lag spectra, the hardening of the power density spectra and the narrowing of the autocorrelation function with increasing photon energy. The model assumes that (i) there is a magnetic field along the axis of the jet, (ii) the electron density in the jet drops inversely proportional to distance, (iii) the jet is “hotter” near its center than at its periphery, and (iv) the electrons in the jet follow a power-law distribution function. We have performed Monte Carlo simulations of Compton upscattering of soft photons from the accretion disk and have found power-law high-energy spectra with photon-number index in the range 1.5–2 and cutoff at a few hundred keV, power-law time lags versus Fourier frequency with index 0.8, and an increase of the rms amplitude of variability and a narrowing of the autocorrelation function with increasing photon energy as they have been observed in Cygnus X-1. The spectrum at long wavelengths (radio, infrared, optical) is modeled to come from synchrotron radiation of the energetic electrons in the jet. We find flat to inverted radio spectra that extend from the radio up to about the optical band. For magnetic field strengths of the order 10⁵–10⁶ G at the base of the jet, the calculated spectra agree well in slope and flux with the observations.     

一种基于UML活动图模型的系统测试方法

UML活动图是基于UML开发的软件设计模型的重要组成部分,它描述了软件系统的动态行为,是软件系统测试过程中的一个重要的信息来源.提出了一个基于UML活动图的场景测试方法,给出了生成基本流和备选流的原则,对传统场景法进行了改进,避免了测试场景集数量爆炸.最后重点结合一个实例对该方法进行了论述.     

太阳光谱辐射强度变化对地球能量平衡的影响分析

目前太阳对地球能量平衡影响的研究大都是以太阳总辐射通量密度作为输入参数的. 本文以美国航空航天局（National Aeronautics and Space Administration,NASA）太阳辐射与气候实验项目的卫星实测数据为基础,对太阳上升相（2010年上半年）和下降相（2007年12月）期间太阳光谱变化对地球能量平衡的影响进行了研究. 结果表明,2010年上半年较强的太阳总辐射通量密度主要是由紫外及红外波段的能量增强引起的,其在200～400nm 和760～4000nm波段内的平均能量分别增加了0.11%和0.05%,而在 400～760nm可见光区的能量却呈减小趋势,平均减小量为0.05%. 通过对MLS2.2全球臭氧日数据进行再分析后发现,相对于2007年12月,2010年上半年平流层臭氧浓度也有所增加,其中在太阳紫外辐射呈现较大增强的2月和3月,其臭氧增量也相对较大,最大值分别出现在33km和40km处,值为0.6mL·m^-3和0.62mL·m^-3. 因此,可见光区能量减弱与平流层臭氧浓度增加的双重削弱作用致使虽然2010年上半年的太阳总辐射通量密度较大,但是到达对流层顶的太阳辐射却有所减小,最大减小量出现在3月,值为0.15W·m^-2. 这一结果说明,太阳活动或总辐射通量密度的增强也有可能对地球对流层系统起到冷却作用.     

航空机电系统技术发展综述

文中总结了国际航空机电系统技术研究现状,以美国为代表的国际先进飞机研发体系,将机电系统技术提升至与飞机平台技术并重的地位,将综合推进、能源与热管理技术列为核心技术领域,持续开展了MEA、INVENT、INPPAT、AVEM、NGT-PAC等一系列面向机电领域的重大技术专项和演示验证计划;梳理了系统架构综合化、能源利用多电化、能量管理高效化的机电系统技术发展趋势;展开了机电系统技术研发思考,提出了强化机电系统技术发展规律和需求认识、升级机电系统技术基础研究,和仿真验证能力是引领机电系统技术发展的2个关键方向。     

Study of the variability of blazars gamma-ray emission

The γ-ray emission of blazar jets shows a pronounced variability and this feature provides limits to the size and to the speed of the emitting region. We study the γ-ray variability of bright blazars using data from the first 18 months of activity of the Large Area Telescope on the Fermi Gamma-Ray Space Telescope. From the daily light-curves of the blazars characterized by a remarkable activity, we firstly determine the minimum variability time-scale, giving an upper limit for the size of the emitting region of the sources, assumed to be spheroidal blobs in relativistic motion. These regions must be smaller than ∼10⁻³ parsec. Another interesting time-scale is the duration of the outbursts. We conclude that they cannot correspond to radiation produced by a single blob moving relativistically along the jet, but they are either the signature of emission from a standing shock extracting energy from a modulated jet, or the superposition of a number of flares occurring on a shorter time-scale. We also derive lower limits on the bulk Lorentz factor needed to make the emitting region transparent for gamma-rays interacting through photon–photon collisions.     

Modeling the broadband persistent emission of magnetars

In this paper, we discuss our first attempts to model the broadband persistent emission of magnetars within a self-consistent, physical scenario. We present the predictions of a synthetic model that we calculated with a new Monte Carlo 3D radiative code. The basic idea is that soft thermal photons (e.g. emitted by the star surface) can experience resonant cyclotron upscattering by a population of relativistic electrons treated in the twisted magnetosphere. Our code is specifically tailored to work in the ultra-magnetized regime; polarization and QED effects are consistently accounted for, as well different configurations for the magnetosphere. We discuss the predicted spectral properties in the 0.1–1000 keV range, the polarization properties, and we present the model application to a sample of magnetars soft X-ray spectra.     

The beaming of external Compton emission

We consider a relativistically moving blob consisting of an isotropic electron distribution that Compton-scatters photons from an external isotropic radiation field. We compute the resulting beaming pattern, i.e. the distribution of the scattered photons, in the blob frame as well as in the observer’s frame by using the full Klein–Nishina cross section and the exact incident photon distribution. In the Thomson regime the comparison of our approach with Dermer (1995) results in concurrent characteristics but different absolute number of the scattered photons by a factor of f_corr = 3.09. Additionally, our calculation yields a slightly lower boost factor which varies the more from the corresponding value in Dermer (1995) the higher the spectral index p of the electron distribution gets.     

Results of solar observations by the CORONAS-F payload

The CORONAS-F mission experiments and results have been reviewed. The observations with the DIFOS multi-channel photometer in a broad spectral range from 350 to 1500 nm have revealed the dependence of the relative amplitudes of p-modes of the global solar oscillations on the wavelength that agrees perfectly well with the earlier data obtained in a narrower spectral ranges. The SPIRIT EUV observations have enabled the study of various manifestations of solar activity and high-temperature events on the Sun. The data from the X-ray spectrometer RESIK, gamma spectrometer HELICON, flare spectrometer IRIS, amplitude–temporal spectrometer AVS-F, and X-ray spectrometer RPS-1 have been used to analyze the X- and gamma-ray emission from solar flares and for diagnostics of the flaring plasma. The absolute and relative content of various elements (such as potassium, argon, and sulfur) of solar plasma in flares has been determined for the first time with the X-ray spectrometer RESIK. The Solar Cosmic Ray Complex monitored the solar flare effects in the Earth’s environment. The UV emission variations recorded during solar flares in the vicinity of the 120-nm wavelength have been analyzed and the amplitude of relative variations has been determined.