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     

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.     

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.     

圆化处理法制备高效大尺寸多晶黑硅太阳电池

采用金属辅助化学腐蚀法制备了多晶黑硅,并研究了极低浓度NaOH溶液对扩孔后黑硅结构的圆化作用及其对多晶黑硅太阳电池性能的影响。用扫描电镜(Scanning electron microscope,SEM)和量子效率(Quantum efficiency, QE)测试仪对黑硅表面形貌及黑硅电池性能进行了表征。结果表明,利用极低浓度的NaOH圆化扩孔后黑硅的尖端及棱角可以减少表面复合的影响。处理后的黑硅表面孔洞均匀且平滑,黑硅太阳电池400~900 nm可见光波段平均反射率为4.15%,批量生产的电池平均转换效率达到17.94%,比常规酸制绒工艺制备的电池平均转换效率提高了0.35%。     

纳米隔热材料的热导率变化规律

为认识和掌握纳米隔热材料的热导率变化规律,以正硅酸乙酯(TEOS)为硅源、炭黑为遮光剂、石英纤维为增强体,采用溶胶-凝胶工艺结合超临界干燥技术制备了纳米隔热材料,并采用热导率测试仪、N_2吸附-脱附、SEM、激光粒度仪对材料进行了表征。测试结果表明:未添加炭黑的材料常压热导率随表观密度的变化以203 kg/m^3为分界点,分界点之前随表观密度的增大线性降低,分界点之后则随表观密度的增大线性升高,并且后一阶段较前一阶段变化快。孔隙率相同时,常压热导率随炭黑含量的增加先降低后稍有升高,极限真空热导率逐渐降低,而常压条件下的气相热导率增大。在半对数坐标系中,气相热导率随环境气压的下降而降低,并且依据降低速率可以划分为三个阶段,101.325～30 kPa之间下降最快,且变化值约为6 mW/(m·K);30～0.1 kPa之间下降较快,且变化值约为2 mW/(m·K);0.1～0.01 kPa之间下降最慢,且基本可以忽略不计。材料常压热导率最低值为16.62 mW/(m·K),添加5wt%的炭黑后可以进一步降低至14.50 mW/(m·K)。     

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 micro-wave 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 obvi-ous 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 di-electric 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.     

三种碳物质对RDX-CMDB推进剂热分解的影响

利用压力ＤＳＣ研究了７ＭＰａ时Ｃ６０、富勒烯烟炱（ＦＳ）和炭黑（ＣＢ）对催化的ＲＤＸ－ＣＭＤＢ推进剂热分解特性的影响。结果表明：使推进剂表现分解热愈大的碳物质，则导致推进剂的燃速愈高。和参比推进剂相比，含ＦＳ的推进剂表现分解热大，故燃速也高，增速作用亦大。不同碳物质导致推进剂表观分解热增加率的大小顺序为：ＦＳ〉ＣＢ〉Ｃ６０。