单阳膜电渗析处理草浆黑液碱回收的研究

为有效治理草浆黑液的污染 ,提高草浆黑液的综合利用率 ,本文针对碱法草浆黑液的特性 ,对单阳膜电渗析技术回收草浆黑液中残碱的可行性进行了研究。研究结果表明 :采用单阳膜电渗析技术回收草浆黑液中的碱 ,技术上是可行的 ;在本试验条件下 ,碱回收受操作电压、操作时间以及强制搅拌等因素的影响 ;综合考虑选用4 .5 V的操作电压、30 min的处理时间 ,经过处理后 ,黑液中 90 %的碱被有效回收 ,其中电流效率大于 70 % ,每吨回收碱的能耗为 4 2 0 0 k W· h左右     

屏幕拟合法在平面连杆机构离散点轨迹综合中的应用

屏幕拟合法是基于轨迹图谱、图形逼近理论及计算机可视化技术的一种平面连杆机构离散点轨迹综合的新方法。用三次B样条曲线将离散点拟合成连续的目标曲线。通过连杆曲线图谱，先初选一个与目标曲线形状接近的连杆曲线，通过调整连杆机构的尺寸参数和图形变换，改变连杆曲线的形状和位置．使其与目标曲线逐渐逼近，直到用肉眼观察完全重合为止。将连杆机构与目标曲线同时放大，在放大状态下再次调整机构参数和对图形进行变换，使两条曲线继续逼近，如果拟合误差满足精度要求则输出设计结果，否则重复上述过程，直到满足精度要求为止。此方法可用来满足任何形状和精度的轨迹拟合要求。     

Study on Microwave Dielectric Property of Carbon Black and Short Carbon Fibers

Carbon black and carbon fibers of different lengths were introduced in different matrices at different ratios to explore their microwave dielectric properties under 8.2 GHz-12.4 GHz. It is found that the actual dielectric constants of the samples containing carbon black are in a two-order function of the contents of carbon black （ε＇, ε＂=Av2＋Bv＋C） and the complex dielectric constants show an obvious frequency response. Of the added fibers of different lengths, the 4 mm-long one could well disperse in the matrices having not only good frequency response, but also larger real parts, imaginary parts and loss values. The imaginary parts and the loss values （tanδ）of the samples with 4 mm-long carbon fibers added increase linearly with the contents of fiber increasing. So it is practicable to adjust the dielectric parameters of the material in a wide range by changing the added amount of carbon black, and the carbon fiber or altering the lengths of the carbon fiber added.     

Optical pre-nova identification for the X-ray Nova GRO J0422+32 (Nova Persei, 1992)

The X-ray Nova GRO J0422+32 in its low brightness has been identified with a B 21 ^m , R20 ^m star on Palomar Sky Survey glass copies. The scans obtained with an automatical microdensitometer along with our special PC program were used. The resulting outburst amplitude 8 ^m is one of similarity features for the class of the low mass X-ray Novae, black hole candidates.     

火星太阳电池翼除尘方法综述

“萤火一号”火星探测器即将发射升空,标志着我国火星探测计划实施的开始。然而,火星尘埃在范德华力和静电力的作用下积聚在太阳电池翼的表面,使其转换效率下降,影响火星探测器的寿命。因此,开展火星太阳电池翼除尘技术的研究是非常有意义的。文章主要介绍了火星太阳电池翼的除尘方法,特别是目前最受关注的电帘除尘方法,并对其基本结构、除尘原理、除尘效率和透光性做了详细的描述,对开展火星太阳电池翼除尘技术的研究具有一定的参考作用。     

Dark energy,co-evolution of massive black holes with galaxies,and ASTROD-GW

The detection of low frequency band (100 nHz–100 mHz) and very low frequency band (300 pHz–100 nHz) gravitational waves (GWs) is important for exploration of the equation of state of dark energy and the co-evolution of massive black holes (MBHs) with galaxies. Most galaxies are believed to have a massive black hole in the galactic core. In the formation of these black holes, merging and accretion are the two main processes. Merging of massive black holes generate GWs which could be detected by space GW detectors and Pulsar Timing Arrays (PTAs) to cosmological distances. LISA (Laser-Interferometric Space Antenna) is most sensitive to the frequency band 1 mHz–100 mHz, ASTROD-GW (ASTROD [Astrodynamical Space Test of Relativity using Optical Devices] optimized for Gravitational Wave detection) is most sensitive to the frequency band 100 nHz–1 mHz and PTAs are most sensitive to the frequency band 300 pHz–100 nHz. In this paper, we discuss the sensitivities and outlooks of detection of GWs from binary massive black holes in these frequency bands with an emphasis on ASTROD-GW. The GWs generated by the inspirals, merging and subsequent ringdowns of binary black holes are standard sirens to the cosmological distance. Using GW observations, we discuss the methods for determining the equation of state of dark energy and for testing the co-evolution models of massive black holes. ASTROD-GW is an optimization of ASTROD to focus on the goal of detection of GWs. The mission orbits of the 3 spacecraft forming a nearly equilateral triangular array are chosen to be near the Sun-Earth Lagrange points L3, L4 and L5. The 3 spacecraft range interferometrically with one another with arm length about 260 million kilometers. With 52 times longer in arm length compared to that of LISA, the strain detection sensitivity is 52 times better toward larger wavelength. The scientific aim is focused for gravitational wave detection at low frequency. The science goals include detection of GWs from MBHs, and Extreme-Mass-Ratio Black Hole Inspirals (EMRI), and using these observations to find the evolution of the equation of state of dark energy and to explore the co-evolution of massive black holes with galaxies.     

Time dependent accretion onto a black hole in a disk plus corona system

Hard X-ray lightcurves exhibit delays of 1 s with respect to the soft X-ray lightcurves when the microquasar GRS 1915+105 is in the state of frequent, regular outbursts. Such outbursts are supposed to be driven by the radiation pressure instability of the inner disk parts. The hard X-ray delays are then caused by the time needed for the adjustment of the corona to changing conditions in the underlying disk. We support this claim by the computation of the time evolution of the disk, including a non-stationary evaporation of the disk and mass exchange with the corona.     

X-ray timing beyond the Rossi X-ray Timing Explorer

With its ability to look at bright galactic X-ray sources with sub-millisecond time resolution, the Rossi X-ray Timing Explorer (RXTE) discovered that the X-ray emission from accreting compact stars shows quasi-periodic oscillations on the dynamical timescales of the strong field region. RXTE showed also that waveform fitting of the oscillations resulting from hot spots at the surface of rapidly rotating neutron stars constrain their masses and radii. These two breakthroughs suddenly opened up a new window on fundamental physics, by providing new insights on strong gravity and dense matter. Building upon the RXTE legacy, in the Cosmic Vision exercise, testing General Relativity in the strong field limit and constraining the equation of state of dense matter were recognized recently as key goals to be pursued in the ESA science program for the years 2015–2025. This in turn identified the need for a large (10 m² class) aperture X-ray observatory. In recognition of this need, the XEUS mission concept which has evolved into a single launch L2 formation flying mission will have a fast timing instrument in the focal plane. In this paper, I will outline the unique science that will be addressed with fast X-ray timing on XEUS.     

表面组装技术的应用与发展（下）

本文主要对表面组装技术的特点、表面组装工艺和表面组装技术的现状及发展趋势进行了全面的介绍，并分析了贴片机、网板印刷机、回流焊、波峰焊对表面组装工艺的影响。     

阻尼网特性数值模拟

依靠经验公式和工程估算等传统方法,无法对阻尼网性能进行精确评估.为确定阻尼网压力损失系数和降湍性能,采用计算流体力学方法,结合适当的边界条件,对阻尼网进行了模拟.使用数值模拟能够得到不同开孔率阻尼网在不同雷诺数、不同入射方向、不同目数的损失系数,与试验结果更为接近,在30°~45°大角度入射时得到的损失系数更为精确;在入射气流与阻尼网平面呈一定夹角时,阻尼网后的气流压力和速度呈现脉动趋势,传播距离大约为100d;在雷诺数小于40时流动保持层流状态,扰动传播距离为50d,此时降湍效果最好,随雷诺数增加,扰动传播距离增加至400d;在流动未失稳时,开孔率越低,降湍效果越明显,开孔率低于0.5时流动容易失稳;开孔率保持不变,随目数增加阻尼网损失系数增加明显,降湍能力提升.因此可以根据数值模拟结果选择阻尼网的最优参数.