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.     

铝合金厚板搅拌摩擦焊焊缝疏松缺陷形成机理

采用圆锥形搅拌头焊接20mm厚的7075-T6铝板,分析焊接过程中焊缝内部疏松缺陷的形成过程及原因。研究表明,焊缝表面成形良好,无明显缺陷。但是,在焊缝轴肩区和焊核区之间出现了疏松缺陷。分析认为,焊缝上、下部金属温度差太大,导致其塑性流动行为发生变化是疏松缺陷形成的主要原因。搅拌摩擦焊(FSW)过程中,焊缝上部金属温度较高,而底部温度仍然很低,脱离搅拌针端部的塑化金属在周围冷金属巨大的变形抗力作用下转而沿搅拌针表面往上迁移。到达轴肩区下方汇聚区时,由于轴肩区金属温度高,向下的挤压力太小,导致回迁上来的塑化金属继续往上迁移并冲破轴肩区而沿轴肩边缘溢出形成飞边。汇聚区内没有足够的塑化金属填充、焊缝无法被压实而产生疏松孔洞。通过建立疏松缺陷形成的物理模型,可以更直观地反映出焊缝金属流动形态及缺陷形成过程。     

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.     

静止轨道卫星通信链路的预算与分析

星地链路计算作为卫星通信的重要技术，是卫星通信系统设计的基础和理论依据，直接决定了卫星通信系统的链路通信质量。由于影响卫星链路的因素很多，设计中存在一处不合理即使得整条星地链路不可用，造成巨大的损失。而且在实际设计中无法做到最理想的链路状态，往往需要在某方面有所取舍，这也是链路计算中的一大难点。基于目前国际通用的链路计算方法，将星地链路上下行拆分，独立计算，综合分析，再结合实际工程经验，分析和计算实际工程案例，针对不同的链路配置给出相应合理的设计方法，可作为静止轨道通信卫星星地链路计算分析的参考。     

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.     

基于降维算法和等效杆长的可展结构精度分析

考虑铰链间隙和杆件尺寸误差的不确定性并通过概率统计方法对其进行研究,提出了一种基于单变量降维算法(UDRM)和等效杆长模型的可展结构精度分析方法。利用UDRM将可展结构的精度性能函数解耦为多个杆件尺寸误差的独立作用形式,建立精度分析模型。引入等效杆长模型,等效杆件替代原杆件进行精度计算。将铰链间隙与原始杆件尺寸误差合并到等效杆件的尺寸误差中,同时证明了等效杆长尺寸误差近似服从正态分布。以某卫星可展开天线为算例,结合高斯求积公式求解展开状态下精度指标的分布期望和方差。通过与蒙特卡罗模拟(MCS)和一次二阶矩(FOSM)法计算结果的对比验证了本文精度分析方法的正确性和高效性。     

热障涂层在涡轮叶片应用中的热防护有效性

建立了含热障涂层的涡轮叶片简化传热模型,通过理论推导建立了热障涂层的有效性判据,并基于此进行了热防护有效性分析。理论分析与数值实验表明:由热障涂层带来的复合传热表面传热系数的变化会显著影响热障涂层的热防护效果；在发动机典型工况下,对于处于高温区的高压涡轮叶片前缘处,热障涂层引起的复合传热表面传热系数变化率最大值的范围为1.25%~10.83%以满足热防护有效性要求。在工程中应特别注意由于热障涂层的应用带来的复合传热表面传热系数的变化,否则会导致热防护失效,甚至产生反效果。      

新一代机载悬挂物管理系统需求分析

针对当前悬挂物管理系统的局限性,结合国外先进战机悬挂物管理系统功能,对我国下一代机载悬挂物管理系统需求进行分析,从FC总线技术、开放式系统架构、多挂点混挂技术、悬挂发射装置控制技术、武器数据链技术5个方面进行了具体的描述,为悬挂物管理系统设计指明了方向.     

前向数据接入方式对导航星座网络通信性能的影响分析

对采用时分多址轮询建链体制的导航星座星间链路网络，为了指导星间链路网络地面前向数据接入的应用，分析了不同地面前向数据接入方式的星-星-地联合数据交互机制及其对网络通信性能的影响，并结合应用代价给出了综合评价和使用建议。以前向数据最快路径接入方式和固定节点接入方式为代表，分析了星间链路网络与地面间星 星 地联合数据交互机制的特点，明确了两种方式下星间链路网络拓扑路由规划策略的制定原则。通过构建Walker 24/3/1导航星座星间链路网络数据处理模型及典型星地运行场景，对两种地面前向数据接入方式仿真分析了星间链路通信容量和传输时延等网络通信性能，比较分析了通信容量及数据拥塞规律，得出前向数据最快路径接入方式相比于固定节点接入方式在通信性能上有较明显优势的结论。最后，综合给出了两种星 星 地联合数据交互机制的应用性评价,同时给出了在通信容量较低且通信时延要求不高、但可靠性要求较高的应用条件下，可适度采用固定节点接入方式的建议。     

Moderate geomagnetic storms and their ionospheric effects at middle and low latitudes

This paper reports the global response of the mid high and low latitude ionosphere in four longitudinal sectors to two moderate geomagnetic storms that occurred during 2007 (the more intense storms occurred that year). The results obtained during these storms show that the ionospheric effects in general are not moderate in magnitude, showing an important degree of complexity as during intense storms. The outstanding features produced during the storms are significant positive storm effects at mid-high latitudes during the main phase/first part of the recovery, positive effects after the onset of the storm followed by negatives effects at middle latitudes and delayed positive effects during the night-time hours in the trough of the equatorial anomaly (“dusk” effect). Possible physical mechanisms for controlling the morphology of the ionosphere during these events are considered.