超高纯氙去除氪低温精馏塔HYSYS模拟优化

为满足大型暗物质探测器PandaX-4T低本底及高灵敏度的要求,探测介质氙(Xe)中氪(Kr)含量要求为n_(Kr)/n_(Xe)≤1×10~(-13)(n为物质的量).本文以超高纯氙去除氪低温精馏塔为例,首先简单介绍精馏塔及其结构设计.其次,对该塔的精馏塔参数进行HYSYS模拟及优化,得出现有运行工况下精馏塔内压力、温度以及氪浓度的分布,并研究了进料位置、回流比、进料流量、再沸器加热量、废品氙流量及进料压力等操作因素对精馏纯度的影响.提出优化提纯效果的精馏操作参数,即塔压为221 kPa、回流比为145时,原料氙中氪含量可从5×10~(-7)提纯到4.1×10~(-14),这对超高纯氙去除氪低温精馏的产品纯度进一步提高有重要指导意义.     

PandaX-4T超高纯氙去除氪低温精馏系统运行分析

PandaX-4T实验组通过McCabe-Thiele(M-T)方法及质量、能量守恒,设计研制出将商业氙中氪的摩尔分数由5×10~(-7)降低至1×10~(-14)的高效低温精馏系统.该超高纯氪氙低温精馏系统已完成离线提纯运行,现需要对其运行状态进行深入分析.通过对系统各个运行阶段的温度、压力、流量及产品氙的摩尔分数等参数进行分析,研究该超高纯氪氙低温精馏系统的稳定性和提纯性能.该低温精馏系统在回收率为99%、提纯速率为10 kg/h的条件下稳定运行1.5 m,共提纯5.75 t氙.实验数据表明,系统在各运行阶段状态稳定、安全可靠,产品氙中氪的摩尔分数小于7.99×10~(-12).PandaX-4T超高纯氪氙低温精馏系统的运行分析具有理论研究价值和工程实际意义,同时也是优化下一阶段精馏提纯运行非常重要的参考依据.     

基于液氙的暗物质直接探测

对暗物质的直接探测是探索暗物质本性的一个重要手段.近年来,随着液氙探测技术的发展,探测质量不断增大,对暗物质的探测灵敏度也不断提高.本文从暗物质在液氙探测器中预期的事例数出发,介绍了液氙探测器的信号产生和关键探测技术,以及控制探测器中本底的方法.目前液氙探测技术对暗物质与核子弹性散射截面的上限已经达到了10-44cm2,今后几年的灵敏度会继续提高2～3个数量级,对暗物质新物理模型做出更好的限制.     

暗物质粒子探测卫星及邻近的电子宇宙射线源

在中国科学院空间科学战略性先导科技专项的支持下,紫金山天文台等单位正在建造"暗物质粒子探测卫星"(DAMPE),预期将于2015年底发射升空.暗物质粒子探测卫星是一个高能伽玛射线、宇宙线探测器,有望在1-10 TeV的电子宇宙射线能谱测量以及GeV-TeV伽玛射线线谱搜寻方面取得重要进展.在本文中,我们扼要介绍暗物质粒子探测卫星探测器的主要组成及功能,并介绍紫金山天文台的科学组在邻近电子宇宙射线源方面的研究进展.     

1000吨/年甘氨酸生产母液中甲醇回收新技术

采用具有新型塔内件的高效填料塔技术，将甲醇回收率提高到９８％以上，甲醇纯度可达９９．８％。同时采用连续水蒸汽直接加热的精馏技术，提高了精馏热效率，节约了热能消耗，生产成本显著降低。应用本技术可创效益近９０万元／年     

对新型填料塔使用的几点看法

精馏是化工生产中最常用的一种分离方法,一般精馏过程耗能较大,并很难分离挥发度相近的混合物,利用新型填料塔可解决这一问题。本文现对国内新型高效填料建造和改造提出几点看法。     

空分精馏过程的仿真计算

从Hamens物性方程出发，依据Or-Ar-N2三元物系气-液平衡关系，对通用模型塔建立统一的数学模型和求解方法，在此基础上开发了空分单塔及精馏系统的计算模型并对填料塔精馏过程进行了探讨和计算．通过宝钢5#空分精馏系统的模拟计算，说明该模型能够准确地描述精馏过程各参数变化．     

间歇精馏过程动态特性及优化操作研究

本文研究间歇精馏过程特定的动态特性,使优化操作方式简单、可靠。在C—02型金属网波填料塔进行乙醇-水系统间歇精馏实验表明:恒回流操作是该塔的优化操作方式。     

精馏硝化法制造TNT新工艺中关于MNT—DNT真空精馏分离的研究

精馏-硝化法是把甲苯硝化成TNT的一种新工艺。 本工艺利用近代高效的金属丝网波纹填料分离MNT的三种异构体(邻一、间一、对一),然后用硝硫混酸把邻一或对一MNT硝化成军品TNT,这样可避免亚硫酸钠溶液精制TNT的工序。精馏-硝化法有三个目的: (a)消除红水(它是一种精制工序产生的污染物)。 (b)MNT多种多样的利用。 (c)军民结合。 本报告研究了关于MNT—DNT精馏分离中的安全问题。藉助于精馏操作基本原理及高效的金属丝网波纹填料的低阻力可设计一套分离装置。通过实验室的试验和在9395厂中间试验的发现,DNT在塔釜中的浓度可以突破美国专利3620928[1]提出的爆炸极限值(10％),即MNT-DNT的分离工艺是安全的。结果为精馏-硝化法扫除了技术上的障碍。     

微分模型用于醋酸甲酯催化精馏水解中试过程的模拟计算

用微分模型对醋酸甲酯催化精馏水解中试过程进行了模拟计算, 反应精馏段催化剂包的气相、液相、液- 固相传质系数和动态持液量用自行测定的经验关联式计算, 提馏段的填料层传质系数用onta 的关联式, 反应速率用自行测定的反应动力学方程式和催化剂包的效率因子进行计算. 模拟计算结果与实验数据吻合良好.     

Adsorption of Xe in zeolite MCM-22

Adsorption of xenon in zeolite MCM-22, a zeolite containing two separate pore systems，has been investigated in detail by variable temperature (VT) ¹²⁹Xe NMR spectroscopy. NMR results suggest that Xe atoms are preferentially adsorbed in the supercages of the zeolite at low Xe pressure (less than a few atmosphere), while Xe atoms can penetrate into the two-dimensional sinusoidal channels at high Xe pressure. Exchange of xenon at the different adsorption sites in the same supercage, i.e. xenon atoms in the two pockets and those in the central part of the supercage, was confirmed at 145 K by two-dimensional (2D) ¹²⁹Xe NMR exchange spectroscopy. The time scale for the exchange is about several milliseconds.     

Seawater subduction controls the heavy noble gas composition of the mantle

The relationship between solar volatiles and those now in the Earth's atmosphere and mantle reservoirs provides insight into the processes controlling the acquisition of volatiles during planetary accretion and their subsequent evolution. Whereas the light noble gases (helium and neon) in the Earth's mantle preserve a solar-like isotopic composition, heavy noble gases (argon, krypton and xenon) have an isotopic composition very similar to that of the modern atmosphere, with radiogenic and (in the case of xenon) solar contributions. Mantle noble gases in a magmatic CO2 natural gas field have been previously corrected for shallow atmosphere/groundwater and crustal additions. Here we analyse new data from this field and show that the elemental composition of non-radiogenic heavy noble gases in the mantle is remarkably similar to that of sea water. We challenge the popular concept of a noble gas 'subduction barrier'--the convecting mantle noble gas isotopic and elemental composition is explained by subduction of sediment and seawater-dominated pore fluids. This accounts for approximately 100% of the non-radiogenic argon and krypton and 80% of the xenon. Approximately 50% of the convecting mantle water concentration can then be explained by this mechanism. Enhanced recycling of subducted material to the mantle plume source region then accounts for the lower ratio of radiogenic to non-radiogenic heavy noble gas isotopes and higher water content of plume-derived basalts.     

Chernobyl radionuclides in a Black Sea sediment trap

The Chernobyl nuclear power station accident released large quantities of vaporized radionuclides, and, to a lesser extent, mechanically released small (less than 1-10 micron) aerosol particles. The total release of radioactivity is estimated to be out of the order of 1-2 x 10(18) Bq (3-5 x 10(7) Ci) not allowing for releases of the xenon and krypton gases. The 137Cs releases of 3.8 x 10(16) Bq from Chernobyl can be compared to 1.3 x 10(18) Bq 137Cs released due to atmospheric nuclear weapons testing. Chernobyl-derived radionuclides can be used as transient tracers to study physical and biogeochemical processes. Initial measurements of fallout Chernobyl radionuclides from a time-series sediment trap at 1,071 m during June-September 1986 in the southern Black Sea are presented. The specific activities of 137Cs, 144Ce and 106Ru in the trap samples (0.5-2, 4-12 and 6-13 Bq g-1) are independent of the particle flux while their relative activities reflect their rates of scavenging in the order Ce greater than Ru greater than Cs.     

A stable argon compound

The noble gases have a particularly stable electronic configuration, comprising fully filled s and p valence orbitals. This makes these elements relatively non-reactive, and they exist at room temperature as monatomic gases. Pauling predicted in 1933 that the heavier noble gases, whose valence electrons are screened by core electrons and thus less strongly bound, could form stable molecules. This prediction was verified in 1962 by the preparation of xenon hexafluoroplatinate, XePtF6, the first compound to contain a noble-gas atom. Since then, a range of different compounds containing radon, xenon and krypton have been theoretically anticipated and prepared. Although the lighter noble gases neon, helium and argon are also expected to be reactive under suitable conditions, they remain the last three long-lived elements of the periodic table for which no stable compound is known. Here we report that the photolysis of hydrogen fluoride in a solid argon matrix leads to the formation of argon fluorohydride (HArF), which we have identified by probing the shift in the position of vibrational bands on isotopic substitution using infrared spectroscopy. Extensive ab initio calculations indicate that HArF is intrinsically stable, owing to significant ionic and covalent contributions to its bonding, thus confirming computational predictions that argon should form a stable hydride species with properties similar to those of the analogous xenon and krypton compounds reported before.     

Gravitational detection of a low-mass dark satellite galaxy at cosmological distance

The mass function of dwarf satellite galaxies that are observed around Local Group galaxies differs substantially from simulations based on cold dark matter: the simulations predict many more dwarf galaxies than are seen. The Local Group, however, may be anomalous in this regard. A massive dark satellite in an early-type lens galaxy at a redshift of 0.222 was recently found using a method based on gravitational lensing, suggesting that the mass fraction contained in substructure could be higher than is predicted from simulations. The lack of very low-mass detections, however, prohibited any constraint on their mass function. Here we report the presence of a (1.9?±?0.1)?×?10(8) M dark satellite galaxy in the Einstein ring system JVAS B1938+666 (ref. 11) at a redshift of 0.881, where M denotes the solar mass. This satellite galaxy has a mass similar to that of the Sagittarius galaxy, which is a satellite of the Milky Way. We determine the logarithmic slope of the mass function for substructure beyond the local Universe to be 1.1(+0.6)(-0.4), with an average mass fraction of 3.3(+3.6)(-1.8) per cent, by combining data on both of these recently discovered galaxies. Our results are consistent with the predictions from cold dark matter simulations at the 95 per cent confidence level, and therefore agree with the view that galaxies formed hierarchically in a Universe composed of cold dark matter.     

Early differentiation and volatile accretion recorded in deep-mantle neon and xenon

The isotopes (129)Xe, produced from the radioactive decay of extinct (129)I, and (136)Xe, produced from extinct (244)Pu and extant (238)U, have provided important constraints on early mantle outgassing and volatile loss from Earth. The low ratios of radiogenic to non-radiogenic xenon ((129)Xe/(130)Xe) in ocean island basalts (OIBs) compared with mid-ocean-ridge basalts (MORBs) have been used as evidence for the existence of a relatively undegassed primitive deep-mantle reservoir. However, the low (129)Xe/(130)Xe ratios in OIBs have also been attributed to mixing between subducted atmospheric Xe and MORB Xe, which obviates the need for a less degassed deep-mantle reservoir. Here I present new noble gas (He, Ne, Ar, Xe) measurements from an Icelandic OIB that reveal differences in elemental abundances and (20)Ne/(22)Ne ratios between the Iceland mantle plume and the MORB source. These observations show that the lower (129)Xe/(130)Xe ratios in OIBs are due to a lower I/Xe ratio in the OIB mantle source and cannot be explained solely by mixing atmospheric Xe with MORB-type Xe. Because (129)I became extinct about 100 million years after the formation of the Solar System, OIB and MORB mantle sources must have differentiated by 4.45 billion years ago and subsequent mixing must have been limited. The Iceland plume source also has a higher proportion of Pu- to U-derived fission Xe, requiring the plume source to be less degassed than MORBs, a conclusion that is independent of noble gas concentrations and the partitioning behaviour of the noble gases with respect to their radiogenic parents. Overall, these results show that Earth's mantle accreted volatiles from at least two separate sources and that neither the Moon-forming impact nor 4.45 billion years of mantle convection has erased the signature of Earth's heterogeneous accretion and early differentiation.     

暗物质的自然现象和成因机理探析

暗物质粒子产生于宇宙大爆炸,它是由一个兆子和两个次能子合成的独立兆子系。由这种兆子系在本体贝粒子流循环输入或输出的增益过程中构成的五维弥散态络合物,就是暗物质又称暗物质云。暗物质云具有质量、引力,但与磁和光均不发生反应。它只能存在于物质态的负引力空间(惰性空间,第五维空间),并与所在宇宙单元区按相同轨迹运动。在单元区中,显物质和暗物质所占的比例大体相同,两者之间通过能量辐射、爆炸的形式实现质量互为转换。地球与具有阻光特性的暗物质云团在相互运动中相遇,应是冰河期的成因之一,这会给地球生态带来毁灭性的破坏。暗物质中蕴含着巨大的能量。对暗物质这一自然存在如何避害趋利是科技界应该考虑的问题。     

S-process krypton of variable isotopic composition in the Murchison meteorite

Current theories on the origin of the chemical elements explain the abundance of medium-heavy and heavy nuclides to be due to the capture by pre-existing lighter nuclides of free neutrons on either a slow timescale (s-process) or a rapid timescale (r-process). Experimental evidence in support of these theories comes from the analysis of carbonaceous chondrites. In acid-resistant residues of these meteorites a kind of xenon has been found, the isotopic composition of which matches almost perfectly that predicted for s-process xenon. We report data that allow us, for the first time, to derive with reasonable precision the full isotopic spectrum of s-process krypton as well. We show that this s-Kr in a residue from Murchison meteorite did not originate in one single s-process but rather is a mixture of contributions from stellar environments where the density of free neutrons was not the same. The astrophysical conditions under which this Krypton has been produced were distinct from those that have been invoked to explain the Solar System s-process abundance. Similar to the 13C-rich carbon component in an aliquot of the same residue, the s-process Kr from different astrophysical sites has retained its identity during the accumulation and subsequent history of the meteorite.     

中空纤维膜接触器精馏过程传质性能的研究

以乙醇-水体系的精馏分离为研究对象,选用不同装填分率的中空纤维膜组件,研究了中空纤维膜接触器的气液传质性能。结果表明：不同装填分率的中空纤维膜接触器,随着装填分率的减小,壳程膜丝分布更加均匀、传质阻力减小、传质性能提高;乙醇-水体系的精馏传质过程为液膜控制,可通过控制液相传质来改善总传质效果;当装填分率一定时,随着气相速度的增加,总传质系数增大、传质性能增强,且其实际值与理论值存在差异。