Complex wind dynamics and ionization structure in symbiotic binaries
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原位电离质谱英文In-Situ Ionization Mass Spectrometry is a powerful analytical technique that has gained significant attention in recent years due to its ability to provide real-time, high-resolution chemical information from complex samples. This technique combines the principles of mass spectrometry with the ability to generate ions directly from the sample of interest, without the need for extensive sample preparation or separation steps. The resulting data can provide valuable insights into the composition, structure, and dynamics of a wide range of materials, from biological samples to industrial products.One of the key advantages of In-Situ Ionization Mass Spectrometry is its ability to analyze samples in their native state. Traditional mass spectrometry techniques often require the sample to be extracted, separated, and sometimes derivatized before analysis. This can introduce potential artifacts or alter the original sample composition. In contrast, In-Situ Ionization Mass Spectrometry allows the sample to be analyzed directly, preserving its original chemical and physical properties. This is particularly important in the study of complex,heterogeneous, or delicate samples, where sample preparation could potentially disrupt or alter the analytes of interest.The fundamental principle of In-Situ Ionization Mass Spectrometry is the generation of gas-phase ions directly from the sample surface or interface. This is achieved through the use of various ionization techniques, such as Laser Desorption Ionization (LDI), Desorption Electrospray Ionization (DESI), and Atmospheric Pressure Chemical Ionization (APCI), among others. These techniques employ different mechanisms to release and ionize the analytes, making them suitable for a wide range of sample types and applications.Laser Desorption Ionization is a popular in-situ ionization method that utilizes a focused laser beam to desorb and ionize analytes from the sample surface. The laser energy is absorbed by the sample, leading to the rapid desorption and vaporization of the analytes, which are then ionized through various mechanisms, such as photoionization or charge transfer. LDI is particularly useful for the analysis of large biomolecules, such as proteins and peptides, as well as inorganic materials and polymers.Desorption Electrospray Ionization, on the other hand, relies on the use of a charged solvent spray to desorb and ionize analytes directly from the sample surface. The solvent droplets interact with the sample, and the analytes are then extracted and ionized through theelectrospray process. DESI is well-suited for the analysis of a wide range of organic compounds, including pharmaceuticals, metabolites, and environmental pollutants, as it can be performed under ambient conditions.Atmospheric Pressure Chemical Ionization is another in-situ ionization technique that generates ions through the interaction of the sample with a high-energy plasma or corona discharge. The analytes are desorbed from the sample and then subjected to chemical ionization reactions, which can lead to the formation of molecular ions or fragment ions. APCI is particularly useful for the analysis of small- to medium-sized molecules, such as drugs, pesticides, and environmental contaminants.The integration of these in-situ ionization techniques with mass spectrometry has led to the development of powerful analytical platforms that can provide real-time, high-resolution chemical information from complex samples. These platforms often incorporate various sample manipulation and introduction strategies, such as microfluidic devices, robotics, and automated sampling systems, to further enhance the capabilities and throughput of In-Situ Ionization Mass Spectrometry.One of the exciting applications of In-Situ Ionization Mass Spectrometry is in the field of biomedical research and clinicaldiagnostics. By analyzing biological samples, such as tissue sections, cells, or body fluids, researchers can obtain valuable information about the distribution, concentration, and interactions of various biomolecules, including proteins, lipids, and metabolites. This information can be used to identify biomarkers for disease diagnosis, monitor therapeutic response, and gain deeper insights into the underlying pathological processes.In addition to biomedical applications, In-Situ Ionization Mass Spectrometry has also found widespread use in material science, environmental analysis, and industrial process monitoring. For example, the technique can be used to study the chemical composition and degradation of polymers, the presence of contaminants in environmental samples, or the real-time monitoring of chemical reactions and product quality in manufacturing processes.The continued development and refinement of In-Situ Ionization Mass Spectrometry techniques have led to improvements in sensitivity, selectivity, and spatial resolution, further expanding the range of applications and opening up new research frontiers. Ongoing efforts in areas such as miniaturization, multi-modal imaging, and data processing algorithms are aimed at making this powerful analytical tool more accessible, versatile, and user-friendly for a wide range of users and industries.In conclusion, In-Situ Ionization Mass Spectrometry represents a transformative approach to chemical analysis, offering the ability to obtain real-time, high-resolution information from complex samples without the need for extensive sample preparation. Its integration with advanced mass spectrometry instrumentation and sample manipulation strategies has led to a growing number of applications in diverse fields, from biomedical research to industrial process monitoring. As this technology continues to evolve, it is poised to play an increasingly important role in our understanding of the chemical world around us and in the development of innovative solutions to complex challenges.。
风能/wind energy 空气流动所具有的能量。
风能资源/wind energy resources 大气沿地球表面流动而产生的动能资源。
空气的标准状态/standard atmospheric state 空气的标准状态是指空气压力为101 325Pa,温度为15℃(或绝对288.15K),空气密度1.225kg/m 3 时的空气状态。
风速/wind speed 空间特定点的风速为该点空气在单位时间内所流过的距离。
平均风速/average wind speed 给定时间内瞬时风速的平均值。
年平均风速/annual average wind speed 时间间隔为一整年的瞬时风速的平均值。
最大风速/maximum wind speed 10分钟平均风速的最大值。
极大风速/extreme wind speed 瞬时风速的最大值。
阵风/gust 超过平均风速的突然和短暂的风速变化。
年际变化/inter-annual variation 以30年为基数发生的变化。
风速年际变化是从第1年到第30年的年平均风速变化。
[风速或风功率密度]年变化/annual variation 以年为基数发生的变化。
风速(或风功率变化)年变化是从1月到12月的月平均风速(或风功率密度)变化。
[风速或风功率密度]日变化/diurnal variation 以日为基数发生的变化。
月或年的风速(或风功率密度)日变化是求出一个月或一年内,每日同一钟点风速(或风功率密度)的月平均值或年平均值,得到0点到23点的风速(或风功率密度)变化。
风切变/wind shear 风速在垂直于风向平面内的变化。
风切变指数/wind shear exponent 用于描述风速剖面线形状的幂定律指数。
风速廓线/wind speed profile, wind shear law 又称“风切变律”,风速随离地面高度变化的数学表达式。
湍流强度/turbulence intensity 标准风速偏差与平均风速的比率。
大气科学系微机应用基础Primer of microcomputer applicationFORTRAN77程序设计FORTRAN77 Program Design大气科学概论An Introduction to Atmospheric Science大气探测学基础Atmospheric Sounding流体力学Fluid Dynamics天气学Synoptic Meteorology天气分析预报实验Forecast and Synoptic analysis生产实习Daily weather forecasting现代气候学基础An introduction to modern climatology卫星气象学Satellite meteorologyC语言程序设计 C Programming大气探测实验Experiment on Atmospheric Detective Technique云雾物理学Physics of Clouds and fogs动力气象学Dynamic Meteorology计算方法Calculation Method诊断分析Diagnostic Analysis中尺度气象学Meso-Microscale Synoptic Meteorology边界层气象学Boundary Layer Meteorology雷达气象学Radar Meteorology数值天气预报Numerical Weather Prediction气象统计预报Meteorological Statical Prediction大气科学中的数学方法Mathematical Methods in Atmospheric Sciences专题讲座Seminar专业英语English for Meteorological Field of Study计算机图形基础Basic of computer graphics气象业务自动化Automatic Weather Service空气污染预测与防治Prediction and Control for Air Pollution现代大气探测Advanced Atmospheric Sounding数字电子技术基础Basic of Digital Electronic Techniqul大气遥感Remote Sensing of Atmosphere模拟电子技术基础Analog Electron Technical Base大气化学Atmospheric Chemistry航空气象学Areameteorology计算机程序设计Computer Program Design数值预报模式与数值模拟Numerical Model and Numerical Simulation接口技术在大气科学中的应用Technology of Interface in Atmosphere Sciences Application海洋气象学Oceanic Meteorology现代实时天气预报技术(MICAPS系统)Advanced Short-range Weather Forecasting Technique(MICAPS system)1) atmospheric precipitation大气降水2) atmosphere science大气科学3) atmosphere大气1.The monitoring and study of atmosphere characteristics in near space as an environment forspace weapon equipments and system have been regarded more important for battle support.随着临近空间飞行器的不断发展和运用,作为武器装备和系统环境的临近空间大气特性成为作战保障的重要条件。
地理科学进展英文版The Progress of Geographical ScienceGeographical science is a multidisciplinary field that studies the Earth's physical features, climate patterns, landforms, ecosystems, human settlements, and their interactions. Over the years, there have been significant advancements in geographical science that have greatly contributed to our understanding of the world. Here are some key areas of progress:1. Remote Sensing and GIS: Remote sensing technology has revolutionized the way we collect data about the Earth's surface. Satellites and airborne sensors provide high-resolution images that help in mapping and monitoring various phenomena such as land use, vegetation cover, and urban growth. Geographic Information Systems (GIS) enable the storage, analysis, and visualization of spatial data, facilitating advanced spatial modeling and decision-making processes.2. Climate Change Research: Geographical science plays acrucial role in studying the impacts of climate change. Scientists analyze temperature records, precipitation patterns, and sea level rise to understand the changing climate and its effects on ecosystems, agriculture, and human societies. This research helps in developing strategies for adaptation and mitigation.3. Geospatial Analysis: Geographical science has seen advancements in geospatial analysis techniques, allowing for more accurate and detailed investigations. Geographic data can be analyzed using statistical methods, spatial interpolation, and geostatistics to identify spatial patterns, trends, and relationships. This aids in solving complex spatial problems, such as disease mapping, urban planning, and transportation optimization.4. Human Geography: The study of human geography has advanced significantly, focusing on the relationships between people and the environment. It includes analyzing population dynamics, migration patterns, urbanization, cultural landscapes, and socioeconomic inequalities. Understanding these factors is crucial for effective urban planning, resource management, and sustainable development.5. Geographical Information Science (GIScience): GIScience is an emerging field that combines geographical science with computer science and artificial intelligence. It explores new methods and algorithms for spatial analysis, data integration, and modeling. GIScience contributes to advancements in location-based services, spatial data mining, and geovisualization techniques.6. Geographical Education: There have been improvements in geographical education, with innovative teaching methods and technologies being adopted. Interactive mapping tools, online data resources, and virtual field trips provide students with hands-on learning experiences and a deeper understanding of geographical concepts.These are just a few examples of the progress made in geographical science. With ongoing advancements in technology and interdisciplinary collaborations, geographical science continues to evolve and contribute to our knowledge of the world around us.。
为了便于一些同学阅读矿井通风与空调方面的英文参考资料和为以后撰写英文论文发表,下面给出了一些常见的矿井通风与空调中英文专业词汇。
Abandoned workings 废弃坑道Absolute pressure 绝对压力Acceptable accuracy 允许精度Active regulation 主动调节(增压调节)Actual characteristic curves实际特征曲线Adiabatic and isentropic processes等熵线绝热的过程Adiabatic saturation process 绝热饱和过程Aerofoils风板Aerosol particles 气溶胶粒子Air crossings 风桥Air mover 鼓风机Air power空气动力Air pressure management 风压管理Air quantity survey空气质量调查Air regulators 风窗Airborne pollutants空气污染物Airflow measurements 风流测定Airflow reversal反向风流Airlock 气闸Airlocks 风门Airway resistance curve风路阻力曲线Alpha, beta and gamma radiation阿尔法、贝塔和伽玛辐射Altimeters 高度计Angular velocity角速度Asbestos 石棉Atkinson equation阿特金森方程式Atmospheric conditions 大气状态Atmospheric pressure 大气压力Auxiliary ventilation 辅助通风Axial fan轴流风机Axial impeller轴向式叶轮Backfill material 充填材料Barometers 气压计Barometric pressure at inlet 入口气压Becquerel (Bq) 贝克勒尔Bernoulli's equation for ideal fluids 理想流体伯努力方程Biot number 比奥数Blackdamp 窒息气体Blast fume炮烟Booster fans 局扇Boreholes 钻孔Branch resistance分支阻力Branch tree分支树Brattice curtain 风帘Brattices 风帘Bronchioles 细支气管Brownian motion 布朗运动Buoyancy (natural draft) effect浮力作用Burying the fire掩埋火源Cage and skip 罐笼和箕斗Carbon dioxide produced生成二氧化碳Carbon dioxide 二氧化碳Carbon monoxide 一氧化碳Carcinogenic (cancer causing) dusts 致癌粉尘Carnot cycle 卡诺循环Centrifugal fan离心风机Centrifugal impeller离心叶轮Chemical absorption化学吸收Chézy-Darcy equation谢兹-达西方程Chilled water spray chamber 冷却液体喷雾室Choke effect瓶颈效应Circular airway 循环风路Closed loop闭环Closed path回路Coal workers' pneumoconiosis (CWP) 煤工尘肺病Coefficient of drag阻力系数Coefficient of dynamic viscosity动力粘度系数Coefficient of friction摩擦系数Compressed air-assisted sprays 压气助喷雾Compressible flow可压缩流Computational fluid dynamics计算流体力学Condenser cooling tower 凝气器降热塔Condenser 冷凝器Consolidation 固结Contaminants 污染物Continuity equation 连续方程Controlled partial recirculation 受控开路循环通风Controlled recirculation in headings 掘进面受控循环通风Convected energy 扩散能Convective heat transfer 对流换热Conveyance运输工具Copper orebody 铜矿体Cross section of a duct or airway 管道或风路断面Curie, Ci 居里Cylindrical cyclone重力旋流器Dealing with a spontaneous heating 处理自热Degrees Celsius 摄氏度Degrees Kelvin绝对温度Density of gases 气体密度Desorption kinetics解吸动力学Dew point hygrometers 露点毛发湿度计Diaphragm gauge 隔膜片仪表Diesel emissions柴油机排放物Diesel exhaust fume柴油机尾气Diesel particulate matter柴油机颗粒物质Differential pressure instruments 微压差计Dimensionless无量刚Disaster management 灾害管理District systems 分区通风系统Dose rates 剂量率Downcast shaft入风井Droplet diameter雾滴直径Duct system风管系统Dust suppression 降尘Dynamic behavior of molecules 分子运动特征Electrochemical methods电化学方法Electrostatic precipitators 电除尘器Emanation of radon 氡的辐射Empirical method 经验方法Energy recovery device 能量回收装置Enthalpy of moist air潮湿空气的焓Enthalpy 焓Entry and exit losses 入口和出口阻力损失Environmental engineering 环境工程Equivalent length当量长度Equivalent resistance等效风阻Equivalent resistance等效阻力Equivalent sand grain roughness相当砂粒粗糙度Escape way 逃生通道;安全通道Euler's equation欧拉方程Evaporator蒸发器Excavating the fire挖掘火源Exhausting air 抽出空气Exhausting system 抽出式通风系统Explosive dusts 爆炸粉尘Explosives炸药Fan characteristic curve风机特征曲线Fan maintenance 风机维护Fan performance 风机性能Fan static pressure风机静压Fan total pressure风机全压Fan velocity pressure风机速度压Fibrogenic dusts 矿渣粉尘Filament and catalytic oxidation (pellistor) detectors丝状催化氧化探测器Fire triangle 火三角Firedamp 甲烷Firefighting with water 以水灭火First law of thermodynamics 热力学第一定律Fixed point measurement固定点测量Fixed quantity branch固定风量分支Flame safety lamps灯具安全火焰Flexible tubing 柔性风筒Flooded orifice scrubber 水淹孔洗涤器Flooding and sealing off 溢出和密封作用Flow work 流动功Fluid mechanics 流体力学Fluid pressure 流体压力Fog 雾Fogged air 雾气Forcing air压入空气Forcing or blowing system 压入式通风系统Fourier number傅里叶数Fragmented rock 破碎岩石Free crystalline silica (quartz, sand stones, flint)游离硅晶体Friction factor摩擦系数Frictional flow 摩擦流动Frictional losses摩擦损失Frictional pressure drop摩擦压降Frictional resistance 摩擦阻力Frictionless manner 无摩擦状态Gas adsorbents 气体吸收剂Gas chromatography气相色谱Gas constants 气体常数Gas drainage 瓦斯抽放Gas laws 气体定律Geothermic gradient 地热梯度Gob drainage采空区抽放气体Grab samples 样品收集Gravitational field 重力场Gravitational settlement of particles 引力沉降颗粒Gravitational settlement 重力沉降Hair hygrometers 毛发湿度计Hardy-Cross technique哈代克劳斯技术Haulage airways 运输风路Haulage level 运输平巷Heat capacity 热容Heat cramps 中暑痉挛Heat diffusivity 热扩散系数Heat exchanger 换热器Heat exchange换热Heat exhaustion 热量消耗Heat fainting 热昏厥Heat flux 热通量Heat illness 中暑Heat rash 热疹Heat stroke 中暑Heat tolerance 耐热性Heat transfer coefficient 传热系数High expansion foam高倍数泡沫High pressure tapping高压测压孔Hoisting shaft提升竖井Hot wire anemometer热线风速仪Hydraulic radius水力半径Hydrogen sulfide硫化氢气Hydrolift system 水力提升系统Hydropower 水电Ice system 冷却系统Ideal gas 理想空气Ideal isothermal compression理想恒温压缩Immediate response 应急反应Induction 感应Industrial Hygienists 工业卫生学家Inhalation rate吸入速度Initiation of explosions引发爆炸Injection of inert gases注射惰性气体Inlet and outlet ducts入口和出口管In-situ measurement 现场测量Intake airway 进风风路Interception and electrostatic precipitation 截留和静电沉淀Interference factor干扰因素Interferometers干涉计Internal Energy 内能Ionization smoke detectors离子感烟探测器Iron pyrites黄铁矿Jet fan 射流风机Junction节点Kata thermometer 卡它计Kinetic energy 动能Kirchhoff's Laws 基尔霍夫定律Laminar and turbulent flow层流和紊流Laminar resistance 层流阻力Laminar sublayer层流次边界层Laser spectroscopy激光光谱学Latent (or hidden) heat of the air空气的潜热Layout of mine 矿井布置Leakage control漏风控制Legislation 法规Level workings阶段工作面Loading station装运站Longitudinal fittings纵向装备Longwall长壁开采法Machine mounted gas monitors悬挂式气体检测器Main fans 主扇Main haulage route主运输道Main return 主(总)回风道Manometers 压差计Mass flow 质量流量Mass spectrometers质谱仪Mean free path 平均自由程Mean velocity of air 平均风速Mesh selection网孔选择Mesh网Metabolic heat balance 代谢热量平衡Metabolic heat代谢热Metal mine fires金属矿井火灾Meteorology 气象Methane drainage瓦斯排放Methane 甲烷Method of mining 采矿方法Mine climate 矿井气候Mine resistance 矿井阻力Mine ventilation 矿井通风Mist eliminator 除雾器Mist 雾Moisture content (specific humidity) of air空气的含湿量Momentum 动量Monitoring systems 监测系统Moving traverses运动线路Natural ventilating effect自然通风影响Natural ventilation 自然通风Neutral skin temperature 中性表皮温度Nikuradse's curves 尼库拉则曲线Nondispersive infra-red gas analyzer非分散红外线气体分析仪Nuisance dusts 粉尘污染Numerical method数值方法Nusselt number努塞尔数Old workings老工作面One standard atmosphere 一个标准大气压Open and concealed fires 明火和隐蔽火灾Ore pass 放矿溜井Ore production矿石生产Orebody deposit 矿体Outbursts from roof and floor 顶板和底板瓦斯突出Overlap systems of auxiliary ventilation 混合式局部通风Oxides of nitrogen氧化氮Oxygen Consumption耗氧量Parallel network or circuit并联网络或回路Paramagnetic analyzer 顺磁分析仪Passive regulator 可调风窗Pellistor methanometers瓦斯检定器Peripheral velocity圆周速度Permanent environmental monitors 持久环境监控Permeability 渗透率Personal dosemeters 个人剂量计Personal respirators 个体呼吸器Phases of oxidation氧化反应阶段Photometric (light-scattering) methods 分光光度Physical adsorption物理吸附Physical thermodynamics 物理热力学Pick face flushing and jet-assisted cutting 锯齿面冲洗与喷气助推器切割Piezoelectric instruments 压电仪器Pitot-static tube皮托静压管Polyvinyl chloride (PVC)聚氯乙烯Potential energy 势能Prandtl number 普兰特尔数Precautions against spontaneous combustion自燃预防Pressure energy 压能Pressure head 压头Pressure surveys压力调查Pressure transducers 压力传感器Pressure-volume surveys压力容积测量Profilometer轮廓仪Psychrometric chart 温湿图Psychrometric measurements 干湿度测量Push-pull system 压-抽混合式通风系统Radial velocity径向速度Radiation 辐射Radiative heat transfer 辐射传热Radioactive decay and half-life放射衰变和半衰期Radon daughters氡子体Radon decay constant 氡的衰变常数Radon, Rn氡气Ramp 斜坡道Rates of heat production 生产率Rates of oxygen consumption 氧气消耗率Refrigerant fluid 制冷液Refrigeration cycle制冷循环Refrigeration systems 制冷系统Refuge chambers避难洞室Regulator 调节器Relative humidity and percentage humidity相对湿度和湿度率Removal of dust from air 气体除尘Re-opening a sealed area重开封闭区Respirable dust呼吸性粉尘Respiratory system 呼吸系统Return airway 回风巷Reynolds Number雷诺数Room and pillar房柱式Rotating vane anemometer旋转叶片风速表Rough pipes 粗管Roughness粗糙度Safety and Health 安全卫生Saturation vapor pressure 饱和蒸汽压Sealants密封剂Seals 密闭Second law of thermodynamics 热力学第二定律Self-heating temperature (SHT) 自热温度Self-rescuers 自救器Sensible heat of the air 空气的显热Series network or circuit串连网络或回路Shaft fittings 井筒装备Shaft wall井壁Shear stress 剪切应力Shock loss factor冲击损耗系数Shock losses 冲击损失Short-Term Exposure Limit (STEL) 短时间接触阈限值SI system of units 国际标准单位体系Sigma heat 西格玛热Smoke tube烟筒Smoking and flame safety lamps 烟火安全灯Smooth concrete lined光滑混凝土内衬Specific heat (thermal capacity)比热容Specific heats 比热Spontaneous combustion of sulfide ores硫化矿自燃Spontaneous combustion自燃Spontaneous heating 自热Spot cooler 现场冷却器Spray fan 喷雾风机Steady flow energy equation稳流能量方程Steady flow physical thermodynamics稳流物理热力学Steady-flow thermodynamics 稳定流热力学Stokes' diameter斯托克斯粒径Stoping areas 回采区Stoppings 密闭Subsurface openings 地下空间Subsurface ventilation 地下通风Sulfide dust explosions 硫化矿粉尘爆炸Sulfur dioxide二氧化硫Sulfuric acid vapor硫酸雾Swinging vane anemometer摆动叶片风速表Tangential velocity at outlet出口切向速度Temperature-entropy diagram温熵图Temporary stopping暂时停止Terminal velocities 自由沉降速度The square law平方定律Thermal conductivity of insulation 绝缘导电温度Thermal conductivity导热系数Thermal equilibrium 热平衡Thermodynamic state 热力学状态Thermoluminescent dosemeters (TLD) 热释光剂量计Thermoregulation 体温调节Threshold limit values (TLV) 阈限值Through-flow ventilation 贯穿通风Time-Weighted Average (TWA)时间加权平均Total energy balance 总能量守恒Total shaft resistance 井筒总阻力Tube bundle systems 管束系统Turbulent resistance紊流阻力U tube manometers U型压差计U tube U型管Uncontrolled recirculation 无控循环通风Underground ventilation system 地下通风系统Unloading station卸载站Upcast shaft出风井Uranium mines 铀矿Vasodilation 血管舒张Velocity contour等流速线Velocity limit速度限值Velocity pressures 动压Velometer速度计Ventilation circuit 通风回路Ventilation door 风门Ventilation engineers 通风工程师Ventilation network analysis通风网络分析Ventilation planning 通风设计Ventilation raise 通风天井Ventilation survey team 通风测量术语Ventilation survey通风测量Venturi scrubber文丘里洗涤器Vertex顶点Viscosity 粘度Viscous drag粘性阻力Volume flow 体积流量Volumetric efficiency 容积效率Vortex-shedding anemometer漩涡式风速表Water gauge pressure 水柱压力Water infusion 注水(水封孔)Water mass flowrate 水质量流量Water vapor content 水蒸气含量Wet and dry bulb hygrometers (psychrometers)干湿球温度表Wet bulb thermometer 湿球温度计Wet Kata thermometer湿球卡他温度表Wet scrubbers湿式除尘器Wetting agents 润湿剂Worked-out area采空区Working face工作面Working level month, WLM 工作水平月Working Level 开采水平Zinc blende闪锌矿——上述词汇摘录自:吴超主编。
上外考研翻译硕士英语天文学专业词汇整理分享find 发见陨星finder chart 证认图finderscope 寻星镜first-ascent giant branch初升巨星支first giant branch 初升巨星支flare puff 耀斑喷焰flat field 平场flat field correction 平场改正flat fielding 平场处理flat-spectrum radio quasar 平谱射电类星体flux standard 流量标准星flux-tube dynamics 磁流管动力学f-mode f 模、基本模following limb 东边缘、后随边缘foreground galaxy 前景星系foreground galaxy cluster 前景星系团formal accuracy 形式精度Foucaultgram 傅科检验图样Foucault knife-edge test 傅科刀口检验fourth cosmic velocity 第四宇宙速度frame transfer 帧转移Fresnel lens 菲涅尔透镜fuzz 展云Galactic aggregate 银河星集Galactic astronomy 银河系天文Galactic bar 银河系棒galactic bar 星系棒galactic cannibalism 星系吞食galactic content 星系成分galactic merge 星系并合galactic pericentre 近银心点Galactocentric distance 银心距galaxy cluster 星系团Galle ring 伽勒环Galilean transformation 伽利略变换Galileo 〈伽利略〉木星探测器gas-dust complex 气尘复合体Genesis rock 创世岩Gemini Telescope 大型双子望远镜giant granulation 巨米粒组织giant granule 巨米粒giant radio pulse 巨射电脉冲Ginga 〈星系〉X 射线天文卫星Giotto 〈乔托〉空间探测器glassceramic 微晶玻璃glitch activity 自转突变活动global change 全球变化global sensitivity 全局灵敏度GMC, giant molecular cloud 巨分子云g-mode g 模、重力模gold spot 金斑病GONG, Global Oscillation Network 太阳全球振荡监测网GPS, global positioning system 全球定位系统Granat 〈石榴〉号天文卫星grand design spiral 宏象旋涡星系gravitational astronomy 引力天文gravitational lensing 引力透镜效应gravitational micro-lensing 微引力透镜效应great attractor 巨引源Great Dark Spot 大暗斑Great White Spot 大白斑grism 棱栅GRO, Gamma-Ray Observatory γ射线天文台guidscope 导星镜GW Virginis star 室女GW 型星habitable planet 可居住行星Hakucho 〈天鹅〉X 射线天文卫星Hale Telescope 海尔望远镜halo dwarf 晕族矮星halo globular cluster 晕族球状星团Hanle effect 汉勒效应hard X-ray source 硬X 射线源Hay spot 哈伊斑HEAO, High-Energy Astronomical 〈HEAO〉高能天文台Observatory heavy-element star 重元素星heiligenschein 灵光Helene 土卫十二helicity 螺度heliocentric radial velocity 日心视向速度heliomagnetosphere 日球磁层helioseismology 日震学helium abundance 氦丰度helium main-sequence 氦主序helium-strong star 强氦线星helium white dwarf 氦白矮星Helix galaxy ( NGC 2685 ) 螺旋星系Herbig Ae star 赫比格Ae 型星Herbig Be star 赫比格Be 型星Herbig-Haro flow 赫比格-阿罗流Herbig-Haro shock wave 赫比格-阿罗激波hidden magnetic flux 隐磁流high-field pulsar 强磁场脉冲星highly polarized quasar ( HPQ ) 高偏振类星体high-mass X-ray binary 大质量X 射线双星high-metallicity cluster 高金属度星团;high-resolution spectrograph 高分辨摄谱仪high-resolution spectroscopy 高分辨分光high - z 大红移Hinotori 〈火鸟〉太阳探测器Hipparcos, High Precision Parallax 〈依巴谷〉卫星Collecting SatelliteHipparcos and Tycho Catalogues 〈依巴谷〉和〈第谷〉星表holographic grating 全息光栅Hooker Telescope 胡克望远镜host galaxy 寄主星系hot R Coronae Borealis star 高温北冕R 型星HST, Hubble Space Telescope 哈勃空间望远镜Hubble age 哈勃年龄Hubble distance 哈勃距离Hubble parameter 哈勃参数Hubble velocity 哈勃速度hump cepheid 驼峰造父变星Hyad 毕团星hybrid-chromosphere star 混合色球星hybrid star 混合大气星hydrogen-deficient star 缺氢星hydrogenous atmosphere 氢型大气hypergiant 特超巨星Ida 艾达( 小行星243号)IEH, International Extreme Ultraviolet Hitchhiker〈IEH〉国际极紫外飞行器IERS, International Earth Rotation Service国际地球自转服务image deconvolution 图象消旋image degradation 星象劣化image dissector 析象管image distoration 星象复原image photon counting system 成象光子计数系统image sharpening 星象增锐image spread 星象扩散度imaging polarimetry 成象偏振测量imaging spectrophotometry 成象分光光度测量immersed echelle 浸渍阶梯光栅impulsive solar flare 脉冲太阳耀斑infralateral arc 外侧晕弧infrared CCD 红外CCDinfrared corona 红外冕infrared helioseismology 红外日震学infrared index 红外infrared observatory 红外天文台infrared spectroscopy 红外分光initial earth 初始地球initial mass distribution 初始质量分布initial planet 初始行星initial star 初始恒星initial sun 初始太阳inner coma 内彗发inner halo cluster 内晕族星团integrability 可积性Integral Sign galaxy ( UGC 3697 ) 积分号星系integrated diode array ( IDA ) 集成二极管阵intensified CCD 增强CCD Intercosmos 〈国际宇宙〉天文卫星interline transfer 行间转移intermediate parent body 中间母体intermediate polar 中介偏振星international atomic time 国际原子时International Celestial Reference 国际天球参考系Frame ( ICRF ) intraday variation 快速变化intranetwork element 网内元intrinsic dispersion 内廪弥散度ion spot 离子斑IPCS, Image Photon Counting System 图象光子计数器IRIS, Infrared Imager / Spectrograph 红外成象器/摄谱仪IRPS, Infrared Photometer / Spectro- meter 红外光度计/分光计irregular cluster 不规则星团; 不规则星系团IRTF, NASA Infrared Telescope 〈IRTF〉美国宇航局红外Facility 望远镜IRTS, Infrared Telescope in Space 〈IRTS〉空间红外望远镜ISO, Infrared Space Observatory 〈ISO〉红外空间天文台isochrone method 等龄线法IUE, International Ultraviolet Explorer〈IUE〉国际紫外探测器Jewel Box ( NGC 4755 ) 宝盒星团Jovian magnetosphere 木星磁层Jovian ring 木星环Jovian ringlet 木星细环Jovian seismology 木震学jovicentric orbit 木心轨道J-type star J 型星Juliet 天卫十一Jupiter-crossing asteroid 越木小行星Kalman filter 卡尔曼滤波器KAO, Kuiper Air-borne Observatory 〈柯伊伯〉机载望远镜Keck ⅠTelescope 凯克Ⅰ望远镜Keck ⅡTelescope 凯克Ⅱ望远镜Kuiper belt 柯伊伯带Kuiper disk 柯伊伯盘LAMOST, Large Multi-Object Fibre Spectroscopic Telescope大型多天体分光望远镜Laplacian plane 拉普拉斯平面late cluster 晚型星系团LBT, Large Binocular Telescope 〈LBT〉大型双筒望远镜lead oxide vidicon 氧化铅光导摄象管Leo Triplet 狮子三重星系LEST, Large Earth-based Solar Telescope〈LEST〉大型地基太阳望远镜level-Ⅰcivilization Ⅰ级文明level-Ⅱcivilization Ⅱ级文明level-Ⅲcivilization Ⅲ级文明Leverrier ring 勒威耶环Liapunov characteristic number 李雅普诺夫特征数light crown 轻冕玻璃light echo 回光light-gathering aperture 聚光孔径light pollution 光污染light sensation 光感line image sensor 线成象敏感器line locking 线锁line-ratio method 谱线比法Liner, low ionization nuclear 低电离核区emission-line regionline spread function 线扩散函数LMT, Large Millimeter Telescope 〈LMT〉大型毫米波望远镜local galaxy 局域星系local inertial frame 局域惯性架local inertial system 局域惯性系local object 局域天体local star 局域恒星look-up table ( LUT ) 对照表low-mass X-ray binary 小质量X 射线双星low-metallicity cluster 低金属度星团;low-resolution spectrograph 低分辨摄谱仪low-resolution spectroscopy 低分辨分光low - z 小红移luminosity mass 光度质量luminosity segregation 光度层化luminous blue variable 高光度蓝变星lunar atmosphere 月球大气lunar chiaroscuro 月相图Lunar Prospector 〈月球勘探者〉Ly-α forest 莱曼-α森林MACHO ( massive compact halo object ) 晕族大质量致密天体Magellan 〈麦哲伦〉金星探测器Magellan Telescope 〈麦哲伦〉望远镜magnetic canopy 磁蓬magnetic cataclysmic variable 磁激变变星magnetic curve 磁变曲线magnetic obliquity 磁夹角magnetic period 磁变周期magnetic phase 磁变相位magnitude range 星等范围main asteroid belt 主小行星带main-belt asteroid 主带小行星main resonance 主共振main-sequence band 主序带Mars-crossing asteroid 越火小行星Mars Pathfinder 火星探路者mass loss rate 质量损失率mass segregation 质量层化Mayall Telescope 梅奥尔望远镜Mclntosh classification 麦金托什分类McMullan camera 麦克马伦电子照相机mean motion resonance 平均运动共振membership of cluster of galaxies 星系团成员membership of star cluster 星团成员merge 并合merger 并合星系; 并合恒星merging galaxy 并合星系merging star 并合恒星mesogranulation 中米粒组织mesogranule 中米粒metallicity 金属度metallicity gradient 金属度梯度metal-poor cluster 贫金属星团metal-rich cluster 富金属星团MGS, Mars Global Surveyor 火星环球勘测者micro-arcsec astrometry 微角秒天体测量microchannel electron multiplier 微通道电子倍增管microflare 微耀斑microgravitational lens 微引力透镜microgravitational lensing 微引力透镜效应microturbulent velocity 微湍速度millimeter-wave astronomy 毫米波天文millisecond pulsar 毫秒脉冲星minimum mass 质量下限minimum variance 最小方差mixed-polarity magnetic field 极性混合磁场MMT, Multiple-Mirror Telescope 多镜面望远镜moderate-resolution spectrograph 中分辨摄谱仪moderate-resolution spectroscopy 中分辨分光modified isochrone method 改进等龄线法molecular outflow 外向分子流molecular shock 分子激波monolithic-mirror telescope 单镜面望远镜moom 行星环卫星moon-crossing asteroid 越月小行星morphological astronomy 形态天文morphology segregation 形态层化MSSSO, Mount Stromlo and Siding Spring Observatory斯特朗洛山和赛丁泉天文台multichannel astrometric photometer ( MAP )多通道天测光度计multi-object spectroscopy 多天体分光multiple-arc method 复弧法multiple redshift 多重红移multiple system 多重星系multi-wavelength astronomy 多波段天文multi-wavelength astrophysics 多波段天体物理naked-eye variable star 肉眼变星naked T Tauri star 显露金牛T 型星narrow-line radio galaxy ( NLRG ) 窄线射电星系Nasmyth spectrograph 内氏焦点摄谱仪natural reference frame 自然参考架natural refenence system 自然参考系natural seeing 自然视宁度near-contact binary 接近相接双星near-earth asteroid 近地小行星near-earth asteroid belt 近地小行星带near-earth comet 近地彗星NEO, near-earth object 近地天体neon nova 氖新星Nepturian ring 海王星环neutrino astrophysics 中微子天文NNTT, National New Technology Telescope国立新技术望远镜NOAO, National Optical Astronomical 国立光学天文台Observatories nocturnal 夜间定时仪nodal precession 交点进动nodal regression 交点退行non-destroy readout ( NDRO ) 无破坏读出nonlinear infall mode 非线性下落模型nonlinear stability 非线性稳定性nonnucleated dwarf elliptical 无核矮椭圆星系nonnucleated dwarf galaxy 无核矮星系nonpotentiality 非势场性nonredundant masking 非过剩遮幅成象nonthermal radio halo 非热射电晕normal tail 正常彗尾North Galactic Cap 北银冠NOT, Nordic Optical Telescope 北欧光学望远镜nova rate 新星频数、新星出现率NTT, New Technology Telescope 新技术望远镜nucleated dwarf elliptical 有核矮椭圆星系nucleated dwarf galaxy 有核矮星系number density profile 数密度轮廓numbered asteroid 编号小行星oblique pulsator 斜脉动星observational cosmology 观测宇宙学observational dispersion 观测弥散度observational material 观测资料observing season 观测季occultation band 掩带O-Ne-Mg white dwarf 氧氖镁白矮星one-parameter method 单参数法on-line data handling 联机数据处理on-line filtering 联机滤波open cluster of galaxies 疏散星系团Ophelia 天卫七optical aperture-synthesis imaging 光波综合孔径成象optical arm 光学臂optical disk 光学盘optical light 可见光optical luminosity function 光学光度函数optically visible object 光学可见天体optical picture 光学图optical spectroscopy 光波分光orbital circularization 轨道圆化orbital eccentricity 轨道偏心率orbital evolution 轨道演化orbital frequency 轨道频率orbital inclination 轨道倾角orbit plane 轨道面order region 有序区organon parallacticon 星位尺Orion association 猎户星协orrery 太阳系仪orthogonal transformation 正交变换oscillation phase 振动相位outer asteroid belt 外小行星带outer-belt asteroid 外带小行星outer halo cluster 外晕族星团outside-eclipse variation 食外变光overshoot 超射OVV quasar, optically violently OVV 类星体variable quasar、optically violent variable quasar oxygen sequence 氧序pan 摇镜头parry arc 彩晕弧partial-eclipse solution 偏食解particle astrophysics 粒子天体物理path of annularity 环食带path of totality 全食带PDS, photo-digitizing system、PDS、数字图象仪、photometric data system 测光数据仪penetrative convection 贯穿对流pentaprism test 五棱镜检验percolation 渗流periapse 近质心点periapse distance 近质心距periapsis distance 近拱距perigalactic distance 近银心距perigalacticon 近银心点perimartian 近火点period gap 周期空隙period-luminosity-colour relation 周光色关系PG 1159 star PG 1159 恒星photoflo 去渍剂photographic spectroscopy 照相分光。
专业英语absorption 吸收absolute leth al dose,LD100绝对致死量absolute humi dity 绝对湿度acid depositi on 酸沉降acid rain 酸雨activated slu dge process 活性污泥法active transp ort 主动运输acute toxicit y test 急性毒性试验acceptabledaily intake,ADI 每天容许摄入量accumulation蓄积作用activated carbon 活性碳adenine腺嘌呤additional joint action相加作用administer 给药、染毒aerobic digestion 有氧消化aerosol 气溶胶afforestation绿化allergic reaction 变态反应air 空气air analysis空气分析air-borne pollutant 空气传播污染物air cleaner空气净化器air contaminant 空气污染物air current气流airflow rate气流速度air humidity气湿air ionization 空气离子化air monitoritoring 大气监测air pollution 大气污染airpollutant大气污染物air pollutionindex 大气污染指数air pollutionsurveillancesystem 大气污染监测系统air pollutionlegislation大气污染法规air pressure气压air purification 大气自净作用air quality standard 大气质量标准air sampler 空气采样器air sanitatio n 空气卫生air sterili zation 空气消毒air temperatu re 气温air temperatu re inversion 逆温air velocit y 空气流速alkalinity 碱度alum 明矾aluminium sul fate 硫酸铝Ames test Am es试验ammonia-chlorine process氯胺消毒法ammonia-nirtiter-nitrates三氮anaerobic digestion 无氧消化anemogram风速计anion synthetic detergent阴离子合成洗涤剂antagonism 拮抗试验antergy 对抗作用argyria 银质沉着病artificial illumination 人工照明arsenic 砷artesian aquifer 承压含水层artesian fountain 自流泉artesian well自流井atmosphere compositions 大气组成automobile exhaust 汽车尾气available chlorine 有效氯back-line study 本底调查bacteriological examinationof water水质细菌学检验base-pair substitution 碱基置换benzo(a)pyrene 苯并(a)芘benzene hexachloride,BHC六六六binign tumor 良性肿瘤bioactivation 生物活化bioassay生物鉴定biochemical oxygen demand生化需氧量biodetoxication 生物解毒/生物灭活作用biogeochemicaldisease 生物地球化学性地方病biological fi lter 生物滤池biological ha lf-life 生物半减期biological tr eatment 生物处理biomembrane粘液生物膜biosphere 生物圈biotoxin 生物毒素biotransformat ion 生物转化biotransport 生物转运black-foot disease 黑脚病blank test空白试验bleaching powder 漂白粉blood/gas partition coefficient 血/气分配系数blood-brain barrier 血脑屏障blood placental barrier血-胎盘屏障burning furnace 焚烧炉carcinoma 恶性肿瘤cadmium 镉calcium hypochlorite 漂白粉精cancer 癌carbon monoxide 一氧化碳carbon monoxide poisoning一氧化碳中毒carbon tetrachloride 四氯化碳carcinogenicity 致癌性carcinogenesis致癌作用centralized water supply集中式给水chemical carcinenesis 化学致癌作用chemical carcinogen 化学致癌物chemicalteratogen 化学致畸物chemical mutagen 化学诱变物chemical oxygen consumption 化学耗氧量chemical oxygen demand 化学需氧量chlorination氯化作用chlorinator加氯器chlorine ammonia treatment氯胺处理chlorine content 含氯量chlorine dema nd 需氯量chlorine dosa ge 加氯量chlorine pois oning 氯中毒chlorine resi dual 余氯chlorobenzen e 氯苯chloroform 氯仿chlorophenotha ne,DDT 滴滴涕chromosome ab erration 染色体畸变chronic abstr icted respira tory disease 慢性阻塞性呼吸道疾病chronic toxicity test 慢性毒性试验cilia 纤毛clarification澄清、净化cloth filter布滤器coagulation混凝coagulant 混凝剂coagulation aids 助凝剂cocarcinogen促癌物coeffient ofnatural illumination 自然照度系数coliforms group 大肠菌群collection water supply system 集中式供水系统colorimeter比色计compost 堆肥comprehensiveutilization综合利用conjugation reaction 结合反应consumer 消费者conversion转化cretinism克汀病cyanide 氰化物cytosine 胞嘧啶cumulative coefficient 蓄积系数damp control 防潮daylighting自然采光decomposer 分解者defluoridation除氟degradation reaction 降解反应delayed toxiceffect 迟发性毒作用dental caries龋齿dental fluorosis 氟骨症deport 输送desalination 淡化(除盐)desertificatio n 沙漠化detoxication 解毒作用direct carcin ogen 直接致癌物direct mutage n 直接致突变物distribution 分布disinfection 消毒dissolved oxy gen 溶解氧distllation蒸馏diversity fac tor 不均匀系数DNA repair修复DNA synthesis合成dominant lethal mutationtest 显性致死突变试验dose-effect relationship剂量效应关系dose-responserelationship剂量-反应关系dust 粉尘或尘ecosystem 生态系统ecological balance 生态平衡ecosphere 生态圈effective temperature 有效温度effective size 有效粒径electrodialysis 电渗析法embryotoxicity胚胎毒性endemia 地方病endemic goiter 地方性甲状腺肿endemic fluorosis 地方性氟中毒energy flow能量流动environmentaldeterioration 环境恶化environmentaldisruption环境失调environmentalecology 环境生态学environmentalhealth standard 环境卫生标准environmentalhealth criteria 环境卫生基准environmentalhygiene 环境卫生学environmentalmonitoring环境监测environmentalpollution环境污染environmental program 环境规划environmental protection agency 环境保护局environmenta l quality st andard 环境质量标准environmental quality eva luation 环境质量评价essential ele ments 必需元素eutrophication 富营养化facilitated d iffusion 易化扩散falling dust 降尘fecal innocence treatment粪便无害化处理ferric sulfate 硫酸铁ferric trichloride 三氯化铁ferrous sulfate 硫酸亚铁filtration 过滤fluoride 氟化物fluorine 氟food chain食物链fog 雾forward mutation 正向突变frameshift mutation 移码突变free residualchlorine 游离余氯fume 烟functional accumulation 功能蓄积gene mutation基因突变genotoxic carcinogen 遗传毒性致癌物goitrogen 致甲状腺肿物质green houseeffects 温室效应green housegases 温室气体groundwater地下水guanine 鸟嘌呤hazard 危害heating 采暖heat control 降温hexavalent chromium 六价铬high risk population 高危险人群hospital sewage treatment医院污水处理humic substance /humus 腐殖质hydrocarbons碳氢化合物hygienic stan dard for dom estic drinkin g water 生活饮用水卫生标准idiosyncratic reaction 特异体质反应immediate tox ic effect 速发毒性反应impervious be d 不透水层indirect carc inogen 间接致癌物indirect muta gen 间接致突变物infrared ray 红外线inhalable particulate,IP可吸入颗粒物initiating stage 启动阶段interhalogens卤间化合物iodine deficiency disorder,IDD 碘缺乏病ionosphere电离层irreversibletoxic effect不可逆毒作用Itai-Itai disease 痛痛病Keshan disease 克山病Kashin-Beck disease 大骨节病landfill 填埋lead 铅Legionnaire’s disease 军团病lethal dose,LD 致死剂量lethal concentration,LC 致死浓度50% lethal dose,LD50 半数致死量lighting coefficient 采光系数local toxiceffect 局部毒作用London smog伦敦型烟雾long-term exposure 长期暴露long-term test 长期试验Los Angelessmog 洛杉矶烟雾manganess 锰marsh gas fermentation 沼气发酵mass-spectrometry 质谱分析法material accumulation 物质蓄积material cycle 物质循环maximal tolerance dose,LD0最大耐受量maximum allowable concentr ation,MAC 最高容许浓度median lethal dose 半数致死剂量/浓度mercury 汞metabolic act ivation 代谢活化metabolic tra nsformation代谢转化metabolic sat uration 代谢饱和metaboism 代谢metabolite 代谢产物metal compoun ds 金属化合物mesosphere 电离层methemoglobinemia 正铁血红蛋白血症micronucleus微核minimal effect level 最小有作用剂量minimal lethal dose 最小致死量minamata disease 水俣病mixed function oxidase,MFO混合功能氧化酶mono-oxygenase单氧酶molecular pollutant 分子状污染物municipal refuse 城市垃圾mutagenesis致突变作用mutant 突变体mutagen 致突变物(诱变物)mutagenicty致突变性mutation 突变neurotoxicity神经毒性nitrogen oxides 氮氧化物nitrate 硝酸盐noise protection 防噪声non-genotoxiccarcinogen非遗传毒性致癌物oligodynamicaction 微动作用oncogene 癌基因oxidation 氧化oxidation pond 氧化塘ozone 臭氧ozone depletion 臭氧层耗竭ozone layer臭氧层particulate pollutant 粒子状污染物particle matter,PM 颗粒物percolating w ater 渗滤水pervious bed 透水层persistent or ganic polluta nts(pops) 持续有机污染物pesticide 杀虫剂phagocytosis 吞噬photochemical reaction 光化学反应photochemical smog 光化学烟雾piankton 浮游生物pinocytosis吞饮pollutant standard index,PSI 污染物标准指数polyaluminiumchloride 羟基/碱式氯化铝polyacrylamide,PAA 聚丙烯酰胺point mutation 点突变polychlorinated biphenyls,PCB 多氯联polycyclic Aromatic hydrocarbons,PAH 多环芳烃precarcinogen前致癌物primary environment 原生环境primary pollutant 一次污染物rimary treatment 物理处理/一级处理producer 生产者progressing stage 进展阶段progression进展promoter 促进剂promoting stage 促进阶段promutagen 促诱变物proximate carcinogen 近致癌物pro-oncogene原癌基因public nuisance 公害pulmonary macrophages 肺巨噬细胞purification净化rapid filter快滤池red tide 红潮refuse burner垃圾焚烧炉relative humidity 相对湿度removal of hardness 软化/除硬removal of taste and odo r 除嗅味reversible to xic effect可逆毒作用risk assessme nt 危险度评估reverse osmos is 反渗透法reversional m utation 回复突变sand filtrati on 砂滤sanitary and anti-epidemi c station 卫生防疫站sanitary prot ection of wa ter source水源卫生防护sanitary regulation 卫生法规sarcoma 肉瘤saturated humidity 饱和湿度secondary environment 次生环境secondary pollution 二次污染secondary pollutant 二次污染物secondary treatment 二级处理/生物处理sedimentation沉淀selection ofwater source 水源选择selenium 硒separate water supply 分散式给水septic tank化粪池sewage works污水处理厂sewage irrigation 污水灌溉sick buildingsyndrome,SBS不良建筑物综合症silver 银simple diffusion 简单扩散skeletal fluorosis 氟骨症slow filter慢滤池smog 烟雾self-purification 自净作用soil pollution 土壤污染somatic mutation 体细胞突变SOS chromotest SOS显色试验spectrophotometer 分光光度计septic tand化粪池spontaneous mutation 自发突变storage depot 贮存库stratosphere 平流层stabilization pond 稳定塘subacute toxi city test 亚急性毒性试验subchronic to xicity test 亚慢性毒性试验sun radiation 太阳辐射susceptible p opulation 敏感人群suspending pa rticulate 飘尘sulphur dioxi de 二氧化硫surface water地面水synergistic joint action协同作用systemic toxic effect 全身毒作用target organ靶器官terate 畸胎teratology 畸胎学teratogenic effect 致畸作用teratogenicity致畸性temperature inversion 气温temperature regulation 温度调节tertiary treatment 三级处理/深度处理total organiccarbon,TOC总有机碳total hardness 总硬度total dissolved solids 溶解性总固体total bacteria count 细菌总数tolerance 耐受性toxication 中毒toxicant 毒物toxicity 毒性transition 转换transversion颠换troposphere对流层toxico-dynamics 毒效学toxico-Kinetics 毒物代谢动力学tubidity 浑浊度tumor suppressorgene 抑癌基因unscheduled DNA synthesis,UDS 程序外DNA合成ultimate carcinogen 终致癌物ultraviolet r ay 紫外线visible light 可视线volatile orga nic compounds ,VOCs 挥发性有机物volatile phen olic compound s 挥发酚类waste disposa l 垃圾处理waste recycli ng 废物回收利用waste residue 废渣waste scaveng ing 废物清除wind 气流。
第 12 卷第 12 期2023 年 12 月Vol.12 No.12Dec. 2023储能科学与技术Energy Storage Science and Technology耦合光热发电储热-有机朗肯循环的先进绝热压缩空气储能系统热力学分析尹航1,王强1,朱佳华2,廖志荣2,张子楠1,徐二树2,徐超2(1中国广核新能源控股有限公司,北京100160;2华北电力大学能源动力与机械工程学院,北京102206)摘要:先进绝热压缩空气储能是一种储能规模大、对环境无污染的储能方式。
为了提高储能系统效率,本工作提出了一种耦合光热发电储热-有机朗肯循环的先进绝热压缩空气储能系统(AA-CAES+CSP+ORC)。
该系统中光热发电储热用来解决先进绝热压缩空气储能系统压缩热有限的问题,而有机朗肯循环发电系统中的中低温余热发电来进一步提升储能效率。
本工作首先在Aspen Plus软件上搭建了该耦合系统的热力学仿真模型,随后本工作研究并对比两种聚光太阳能储热介质对系统性能的影响,研究结果表明,导热油和太阳盐相比,使用太阳盐为聚光太阳能储热介质的系统性能更好,储能效率达到了115.9%,往返效率达到了68.2%,㶲效率达到了76.8%,储电折合转化系数达到了92.8%,储能密度达到了5.53 kWh/m3。
此外,本研究还发现低环境温度、高空气汽轮机入口温度及高空气汽轮机入口压力有利于系统储能性能的提高。
关键词:先进绝热压缩空气储能;聚光太阳能辅热;有机朗肯循环;热力学模型;㶲分析doi: 10.19799/ki.2095-4239.2023.0548中图分类号:TK 02 文献标志码:A 文章编号:2095-4239(2023)12-3749-12 Thermodynamic analysis of an advanced adiabatic compressed-air energy storage system coupled with molten salt heat and storage-organic Rankine cycleYIN Hang1, WANG Qiang1, ZHU Jiahua2, LIAO Zhirong2, ZHANG Zinan1, XU Ershu2, XU Chao2(1CGN New Energy Holding Co., Ltd., Beijing 100160, China; 2School of Energy Power and Mechanical Engineering,North China Electric Power University, Beijing 102206, China)Abstract:Advanced adiabatic compressed-air energy storage is a method for storing energy at a large scale and with no environmental pollution. To improve its efficiency, an advanced adiabatic compressed-air energy storage system (AA-CAES+CSP+ORC) coupled with the thermal storage-organic Rankine cycle for photothermal power generation is proposed in this report. In this system, the storage of heat from photothermal power generation is used to solve the problem of limited compression heat in the AA-CAES+CSP+ORC, while the medium- and low-temperature waste heat generation in the organic Rankine cycle power收稿日期:2023-08-18;修改稿日期:2023-09-18。
动力气象学英语Dynamic Meteorology, a branch of atmospheric science, focuses on the study of atmospheric motions and the physical processes that drive weather systems. It is a critical field for understanding the complex interactions between theEarth's atmosphere and the energy that moves through it.At the core of dynamic meteorology is the concept offluid dynamics, which applies the principles of physics to the behavior of gases and liquids. In the atmosphere, these principles help explain how air masses move, how they interact, and how they can lead to the development of various weather phenomena.One of the fundamental equations in dynamic meteorologyis the equation of motion, which describes the movement ofair parcels. This equation takes into account several forces, including the pressure gradient force, Coriolis force, and friction. The pressure gradient force is the primary driver of wind, pushing air from areas of high pressure to areas of low pressure. The Coriolis force, a result of the Earth's rotation, causes moving air to be deflected, which is essential in the formation of large-scale weather systemslike cyclones and anticyclones.Another key aspect of dynamic meteorology is the conservation of energy. The atmosphere is a complex system where different forms of energy, such as potential energy,kinetic energy, and latent heat, are constantly being converted. For example, when air rises and cools, water vapor can condense into clouds, releasing latent heat into the atmosphere and influencing the development of storms.Thermodynamics also plays a significant role in dynamic meteorology. It involves the study of heat and temperature and their effects on the atmosphere. The temperature differences in the atmosphere can lead to convection, which is the process by which warm air rises and cool air sinks, creating circulation patterns in the atmosphere.Dynamic meteorologists use a variety of tools and models to predict and understand weather patterns. Numerical weather prediction (NWP) models are mathematical representations of the atmosphere that simulate its behavior based on initial conditions and physical laws. These models are essential for forecasting weather and are continually being refined to improve their accuracy.In conclusion, dynamic meteorology is a multifacetedfield that combines physics, fluid dynamics, and thermodynamics to study and predict the behavior of the atmosphere. It is a crucial component of modern weather forecasting and plays a vital role in understanding and preparing for the impacts of climate change.。
物理专业英语词汇(G)g factor 朗德 g 因子g value g 值ga al as semiconductor laser 镓铝砷半导体激光器gaas laser 砷化镓激光器gadolinium 钆gage 量规gain 增益gain margin 增益余量gain of antenna 天线增益gal 伽galactic absorption 银河吸收galactic axion 银河轴子galactic background radiation 银河背景辐射galactic center 银心galactic cluster 银河星团galactic concentration 银聚度galactic coordinates 银道坐标galactic corona 银河晕galactic cosmic ray 银河系宇宙线galactic equator 银道galactic halo 银河晕galactic latitude 银纬galactic longitude 银经galactic nebula 银河星云galactic nova 银河新星galactic nucleus 银核galactic plane 银道面galactic pole 银极galactic radio astronomy 银河系射电天文学galactic radio noise 银河射电噪声galactic rotation 银河系自转galactic wind 星系风galaxy 星系galerkin's method 盖勒金方法galilean satellites 伽利略卫星galilean telescope 伽利略望远镜galilean transformation 伽利略变换gallium 镓gallium arsenide 砷化镓gallium arsenide diode 砷化镓二极管gallium arsenide field effect transistor 砷化镓场效应晶体管gallium arsenide laser 砷化镓激光器gallon 加仑galvanic cell 伽伐尼电池galvanic electricity 动电galvanizing 镀锌galvanometer 检疗gamma 伽玛gamma activity 放射性gamma camera 射线照相机gamma decay 衰变gamma emitter 发射体gamma function 伽马函数gamma matrix 矩阵gamma quantum 量子gamma radiography 射线照相法gamma ray absorption 射线吸收gamma ray absorption coefficient 射线吸收系数gamma ray astronomy 射线天文学gamma ray burst 射线闪烁gamma ray detector 射线探测器gamma ray dosimetry 射线剂量测定法gamma ray emission 射线发射gamma ray laser 激光器gamma ray material testing 射线探伤法gamma ray object 射线天体gamma ray scattering 射线散射gamma ray source 发射体gamma ray spectrometer 射线能谱仪gamma rays 射线gamma space 空间gamma spectroscopy 射线能谱学gamma spectrum 谱gamma vibration 振荡gamow teller selection rule 伽莫夫 特勒选择定则gamow teller transition 伽莫夫 特勒跃迁gantmakher effect 甘特马克效应gap 空隙gapless superconductor 无能隙超导体garnet 石榴石garnet structure 石榴石型结构gas 气体gas amplification 气体放大gas ballast vacuum pump 气镇真空泵gas calorimetry 气体量热法gas chromatography 气相色谱法gas constant 气体常数gas cooled fast reactor 气冷快堆gas cooled reactor 气冷堆gas degeneracy 气体退化gas discharge 气体放电gas discharge laser 气体放电激光器gas discharge plasma 气体放电等离子体gas dynamic laser 气动激光器gas dynamics 气体动力学gas flow counter 柳型计数器gas ionization 气体电离gas laser 气体激光器gas manometer 气体压力计gas meter 气量计gas scintillator 气体闪烁器气体闪烁体gaseous diffusion 气体扩散gaseous ion 气体离子gaseous line 气相线gaseous nebula 气体星云gaseous phase 气相gaseous wastes 气态废物gasket 密封垫gate array 门数组gate circuit 门电路gauge 量规gauge fixing 规范固定gauge invariance 规范不变性gauge particles 规范粒子gauge symmetry 规范对称性gauge theory 规范理论gauge transformation 规范变换gauge transformation of the first kind 第一类规范变换gauge transformation of the second kind 第二类规范变换gauss 高斯gaussian approximation 高斯近似gaussian curve 高斯曲线gaussian distribution 正态分布gaussian optics 高斯光学gaussian process 高斯过程gay lussac's law 盖 吕萨克定律geiger counter 盖革计数器geiger nuttall's law 盖革 努塔耳定律geiger region 盖革区geissler tube 盖斯勒管gel 凝胶gell mann low relation 盖尔曼 洛关系gell mann nishijima rule 盖尔曼 魏定则gemini 双子座gene 基因gene engineering 基因工程general astronomy 普通天文学general circulation 环流general precession 总岁差general principle of relativity 广义相对论原理general theory of relativity 广义相对论generalized coordinates 广义坐标generalized eigenvector 广义本崭量generalized flow 广义流generalized force 广义力generalized free field 广义自由场generalized momentum 广义动量generalized thermodynamic force 广义热力学力generating electricity with thermalion 热离子发电generating function 母函数generating process 发生过程generation 世代generator 发电机genetic information 遗传信息geocentric coordinates 地心坐标geocentric parallax 地心视差geocentric theory 地心说geochronology 地质年代学geodesic 测地线geodesic coordinates 测地坐标geodesic curve 测地线geodesic precession 测地线旋进geodesy 测地学geoid 大地水准面geomagnetic activity 地磁活动geomagnetic activity index 地磁指数geomagnetic coordinates 地磁坐标geomagnetic effect 地磁效应geomagnetic field 地磁场geomagnetic inclination 地磁倾角geomagnetic latitude 地磁纬度geomagnetic meridian 地磁子午线geomagnetic pole 地磁极geomagnetic pulsation 地磁脉动geomagnetic storm 磁暴geomagnetic variation 地磁变化geomagnetism 地磁geometric cross section 几何截面geometric resonance 几何共振geometric variable 几何变星geometrical acoustics 几何声学geometrical isomerism 几何异构geometrical libration 几何平动geometrical optics 几何光学geometrical variable 几何变星geometry 几何geometry factor 几何因数geometry of the spectrum 谱几何geophone 地震检波器地音仪geophysical prospecting 地球物理勘探geophysics 地球物理学geopotential 重力势georgi glashow model 居尔吉 格拉肖模型geostrophic current 地转风气流geostrophic wind 地转风geothermal power plant 地热发电厂ger 量子germanium 锗germanium diode 锗二极管germanium rectifier 锗整流germanium semiconductor detector 锗半导体探测器germanium transistor 锗晶体管getter 吸气剂getter pump 吸气剂泵gettering 吸气gev 十亿电子伏特ghost 鬼线ghost image 鬼象giaever tunnelling 杰伯隧道效应giant 巨星giant impact 巨冲击giant planet 巨行星giant pulse 巨脉冲giant pulse laser 巨脉冲激光器giant resonance 巨共振giant star 巨星gibbs distribution 吉布斯分布gibbs duhem relation 吉布斯 迪昂关系gibbs ensemble 吉布斯系综gibbs free energy 吉布斯自由能gibbs helmholtz equations 吉布斯 亥姆霍茨方程gibbs paradox 吉布斯佯谬gibbs phase rule 吉布斯相律giga 吉gigacycle per second 吉周每秒gigaelectronvolt 吉电子伏特gigapascal 吉帕斯卡gilbert 吉伯gim mechanism gim 机制ginzburg landau equation 金兹堡 朗道方程ginzburg landau theory 金兹堡 朗道理论glan foucault prism 格兰 傅科棱镜glan thompson prism 格兰 汤普森棱镜glass 玻璃glass laser 玻璃激光器glass transition 玻璃转化glass transition point 玻璃化转变点glassy metal 金属玻璃glassy state 玻璃态glide plane 滑移面glide reflection 滑移反射glider 滑翔机globar 碳化硅炽热棒globe 球globular cluster 球状星团gloss 光泽glove box 手套箱glow 辉光glow discharge 辉光放电glow lamp 辉光灯glueball 胶子偶素gluodynamics 胶子动力学gluon 胶子gluonium 胶子偶素gnomonic projection 球心投影gns reconstruction theorem gns 改造定理golay cell 戈莱盒gold 金gold leaf electroscope 金箔验电器goldberger treiman relation 戈德堡 特莱曼关系goldstone boson 戈德斯通玻色子goldstone mode 戈德斯通模goldstone theorem 戈德斯通定理goniometer 测角仪good program 良好程序good quantum number 佳量子数gorsky effect 戈尔斯基效应gould belt 古尔德带gp zone gp 区gradation 度grade 度graded index multimode fiber 递级折射率多模式光学纤维gradient 梯度graduated circle 分度弧graduation 分度graetz number 格雷兹数grain 晶粒grain boundary 晶界grain boundary diffusion 晶界扩散grain boundary sliding 晶界滑移grain growth 晶粒生长grain size 粒度gram 克gram atom 克原子gram calorie 克卡gram equivalent 克当量gram force 克重gram molecule 克分子gram weight 克重grand canonical ensemble 巨正则系综grand unified theory 大统一理论granularity 粒度granulation 造粒granule 小颗粒graph 图形graph theory 图论graphic method 图示法graphical representation 图示graphite 石墨graphite structure 石墨结构graphite uranium reactor 铀石墨堆grashof number 格拉晓夫数grating 光栅grating constant 光栅常数grating equation 光栅方程grating spectrograph 光栅摄谱仪grating spectrometer 光栅光谱仪grating spectrum 衍射光谱gravimeter 重力仪gravimetric analysis 重量分析gravimetry 重量测定gravitation 引力gravitation field 引力场gravitational acceleration 重力加速度gravitational anomaly 重力反常gravitational collapse 引力坍缩gravitational constant 引力常数gravitational energy 重力能gravitational field 引力场gravitational force 重力gravitational interaction 引力相互酌gravitational lens 引力透镜gravitational lens effect 引力透镜效应gravitational mass 引力质量gravitational paradox 引力佯谬gravitational potential 引力势gravitational quantum 引力子gravitational radiation 引力辐射gravitational radius 引力半径gravitational shift 引力位移gravitational system of units 重力单位制gravitational unit 重力单位gravitational wave 引力波gravitino 引力微子graviton 引力子gravity 重力gravity anomaly 重力反常gravity correction 重力校正gravity wave 引力波gravothermal catastrophe 重力热力学灾祸gray 戈瑞gray body 灰体gray body radiation 灰体辐射grazing collision 擦边碰撞grazing incidence 切线入射great attractor 巨大吸引子great red spot 红斑great wall 长城green blue laser 蓝绿色激光器green function method 格林函数方法green's function 格林函数greenhouse effect 温室效应greenwich mean time 格林尼治平时greenwich meridian 格林尼治子午线greenwich sidereal time 格林尼治恒星时greenwich time 格林尼治时gregorian calendar 格里历grey atmosphere 灰大气grid 点阵grid control 栅极控制grid current 栅极电流grid detection 栅极检波grid leak 栅漏grid potential 栅极电压grid voltage 栅极电压griffith's inequality 格里菲思不等式grinding 研磨ground state 基态ground state correlation 基态相关grounding 接地group 群group of galaxies 星系群group of transformations 变换群group theory 群论group velocity 群速度growth of crystal 晶体生长growth of grain 晶粒生长grus 天鹤座gt cut gt 切割guage anomaly 规范反常guidance 引导guided missile 导弹guider 导星镜guiding center approximation 导向中心近似guiding telescope 导星镜guinier camera 纪尼厄照相机guinier plot 纪尼厄图gunn diode 冈锭应二极管gunn effect 冈锭应gyration radius 回转半径gyrator 回转器gyrocompass 回转罗盘gyromagnetic 回转磁的gyromagnetic effect 回转磁效应gyromagnetic element 磁旋元件gyromagnetic ratio 回转磁比gyroscope 回转器陀螺仪gyroscopic stabiliser 回转式稳定器gyrostat 回转仪gyrotron 振动陀螺仪。
High harmonic generationPerturbative Harmonic GenerationPerturbative Harmonic Generation is a process whereby laser light of frequency ω and photon energy ħω can be used to generate new frequencies of light. The newly generated frequencies are integer multiples nω of the original light's frequency. This process was first discovered in 1961 by Franken et al.,[1] using a ruby laser, with crystalline quartz as the nonlinear medium.Harmonic generation in dielectric solids is well understood and extensively used in modern laser physics (see second harmonic generation). In 1967 New et al. observed the first third harmonic generation in a gas.[2] In monatomic gases it is only possible to produce odd numbered harmonics for reasons of symmetry. Harmonic generation in the perturbative (weak field) regime is characterised by rapidly decreasing efficiency with increasing harmonic order and harmonics up to the 11th order have been observed under these conditions .[3] This behaviour can be understood by considering an atom absorbing n photons then emitting a single high energy photon. The probability of absorbing n photons decreases as n increases, explaining the rapid decrease in the initial harmonic intensities.High Harmonic Generation (HHG)The first High Harmonic Generation (HHG) was observed in 1977 in interaction of intense COlaser pulses with2plasma generated from solid targets.[4] HHG in gases, far more widespread in application today, was first observed by McPherson and colleagues in 1987,[5] and later by Ferray et al. in 1988,[6] with surprising results: the high harmonics were found to decrease in intensity at low orders, as expected, but then were observed to form a plateau, with the intensity of the harmonics remaining approximately constant over many orders.[7] Plateau harmonics spanning hundreds of eV have been measured which extend into the soft x-ray regime.[8] This plateau ends abruptly at a position called the High Harmonic Cut-off.Properties of High HarmonicsHigh harmonics have a number of interesting properties. They are a tunable table-top source of XUV/Soft X-rays, synchronised with the driving laser and produced with the same repetition rate. The harmonic cut-off varies linearlywhere harmonic generation stops.[9] The saturation with increasing laser intensity up until the saturation intensity Isatintensity can be increased by changing the atomic species to lighter noble gases but these have a lower conversion efficiency so there is a balance to be found depending on the photon energies required.High harmonic generation strongly depends on the driving laser field and as a result the harmonics have similar temporal and spatial coherence properties.[10] High harmonics are often generated with pulse durations shorter than that of the driving laser. This is due to phase matching and ionization. Often harmonics are only produced in a very small temporal window when the phase matching condition is met. Depletion of the generating media due to ionization also means that harmonic generation is mainly confined to the leading edge of the driving pulse.[11]High harmonics are emitted co-linearly with the driving laser and can have a very tight angular confinement, sometimes with less divergence than that of the fundamental field and near Gaussian beam profiles.[12]Semi-classical approach to describe HHGThe maximum photon energy producible with high harmonic generation is given by the cut-off of the harmonic plateau. This can be calculated classically by examining the maximum energy the ionized electron can gain in theelectric field of the laser. The cut-off energy is given by,where U p is the ponderomotive energy from the laser field and I p is the ionization potential.This derivation of the cut-off energy is derived from a semi-classical calculation. The electron is initially treated quantum mechanically as it tunnel ionizes from the parent atom, but then its subsequent dynamics are treated classically. The electron is assumed to be born into the vacuum with zero initial velocity, and to be subsequently accelerated by the laser beam's electric field.The three-step model.Half an optical cycle after ionization, the electron will reverse directionas the electric field changes, and will accelerate back towards theparent nucleus. Upon returning to the parent nucleus it can then emitbremsstrahlung-like radiation during a recombination process with theatom as it returns to its ground state. This description has becomeknown as the recollisional model of high harmonic generation .[13]Some interesting limits on the HHG process which are explained bythis model show that HHG will only occur if the driving laser field islinearly polarised. Ellipticity on the laser beam causes the returningelectron to miss the parent nucleus. Quantum mechanically, the overlap of the returning electron wavepacket with the nuclear wavepacket is reduced. This has been observed experimentally, where the intensity of harmonics decreases rapidly with increasing ellipticity.[14] Another effect which limits the intensity of the driving laser is the Lorentz force. At intensities above 1016 Wcm −2 the magnetic component of the laser pulse, which is ignored in weak field optics, can become strong enough to deflect the returning electron. This will cause it to 'miss' the parent nucleus and hence prevent HHG.References[1]P. A. Franken, A. E. Hill, C. W. Peters, and G. Weinreich, Phys. Rev. Lett. 7, 118 (1961).[2]G. H. C. New and J. F. Ward, Phys. Rev. Lett. 19, 556 (1967).[3]J. Wildenauer, Journal of Applied Physics 62, 41 (1987).[4]N. H. Burnett et al., Appl. Phys. Lett., vol. 31, pp. 172–174, 1977.[5] A. McPherson et al, JOSA B 4, 595 (1987).[6]M. Ferray et al., Journal of Physics B-Atomic Molecular and Optical Physics 21, L31 (1988).[7]X. F. Li, A. L'Huillier, M. Ferray, L. A. Lompre, and G. Mainfray, Physical Review A 39, 5751 (1989).[8]J. Seres et al., Nature 433, 596 (2005).[9]T. Brabec and F. Krausz, Reviews of Modern Physics 72, 545 (2000).[10] A. L'Huillier, K. J. Schafer, and K. C. Kulander, Journal of Physics B Atomic Molecular and Optical Physics 24, 3315 (1991).[11]K. J. Schafer and K. C. Kulander, Physical Review Letters 78, 638 (1997).[12]J. W. G. Tisch et al., Physical Review A 49, R28 (1994).[13]P. B. Corkum, Physical Review Letters 71, 1994 (1993).[14]P. Dietrich, N. H. Burnett, M. Ivanov, and P. B. Corkum, Physical Review A 50, R3585 (1994).Article Sources and Contributors3 Article Sources and ContributorsHigh harmonic generation Source: /w/index.php?oldid=597580326 Contributors: Andrewman327, ArcAngel, Danh, Dratman, EnOreg, John of Reading, Kkmurray,MDSwo, Marj11, Micru, Nihonjoe, Qxz, RHaworth, Zeptosecond, 7 anonymous editsImage Sources, Licenses and ContributorsImage:ThreeStep.png Source: /w/index.php?title=File:ThreeStep.png License: Creative Commons Attribution-Sharealike 3.0 Contributors: MDSwo LicenseCreative Commons Attribution-Share Alike 3.0///licenses/by-sa/3.0/。
“蒸发悖论”在秦岭南北地区的探讨蒋冲;王飞;刘思洁;穆兴民;李锐;刘焱序【摘要】潜在蒸散量(ET0)是大气蒸发的估计值,已经广泛应用于灌溉管理和无实测蒸发资料地区的估算.分析ET0的时空变化是研究水资源对气候变化响应的基础工作,同时对于农业水资源的优化利用也具有重要意义.根据秦岭南北47个气象站1960-2011年逐日数据,利用FAO Penman-Monteith公式计算出各站的潜在蒸散量(ET0),研究了气温、降水与ET0之间的长期变化趋势关系,对导致ET0下降的主要原因进行了讨论,着重对秦岭南北地区是否存在“蒸发悖论”进行验证.结果表明:(1)秦岭南北整体气温经历了先降后升的变化过程,1993年为突变年份,1960-1993年的降温速率和1994-2011年的升温速率均表现出由南向北递减的规律,1960-2011年整体升温速率由北向南递减.(2)1979年和1993年是ET0变化的转折点,以1979和1993为界ET0经历了“升—降—降”的变化阶段.1960-1979年仅汉水流域和巴巫谷地存在“蒸发悖论”现象,1980-1993、1994-2011和1960-2011年3个时段区域整体和各子区均发现了“蒸发悖论”现象.秋季后18a 和52a整体以及冬季前34a和52a整体均存在“蒸发悖论”现象,冬季最为明显.(3)近52年整体降水表现出不显著的下降趋势,相较于年尺度,夏季降水与ET0逆向变化趋势更为明显.(4)年尺度上,太阳辐射(日照时数)下降引起的潜热通量减少是造成ET0下降即“蒸发悖论”现象的主要原因.季节尺度,春季ET0下降的主导因素为风速,其它季节均为太阳辐射(日照时数).【期刊名称】《生态学报》【年(卷),期】2013(033)003【总页数】12页(P844-855)【关键词】秦岭南北;潜在蒸散量;蒸发悖论;气温;降水【作者】蒋冲;王飞;刘思洁;穆兴民;李锐;刘焱序【作者单位】西北农林科技大学资源环境学院,杨凌712100;西北农林科技大学资源环境学院,杨凌712100;中国科学院水利部水土保持研究所,杨凌712100;北京大学遥感与地理信息系统研究所,北京100871;西北农林科技大学资源环境学院,杨凌712100;中国科学院水利部水土保持研究所,杨凌712100;西北农林科技大学资源环境学院,杨凌712100;中国科学院水利部水土保持研究所,杨凌712100;陕西师范大学旅游与环境学院,西安710062【正文语种】中文潜在蒸散量(ET0)是指在一定气象条件下水分供应不受限制时,某一固定下垫面土壤蒸发量和植物蒸腾量的总和,它是实际蒸散量的理论上限,也是计算实际蒸散量的基础,又被称之为参考作物蒸散量[1-4]。
清华大学博士论文编辑排版建议采用的字体、字号与正文段落字号相适应,用Word 2000 编辑数学公式时建议采取如下尺寸定义清华大学博士论文格式样例:芳杂环高分子的高温水解特性与量子化学研究(申请清华大学理学博士学位论文)培养单位:清华大学化学系Array专业:物理化学研究生:易某某指导教师:某甲甲教授某乙乙教授副指导教师:芳杂环高分子的高温水解特性与量子化学研究易某某三号仿宋或华文仿宋请将中文封面左边Experimental and Theoretical Investigations of HydrolyticStability of Aromatic Heterocyclic Polymers in High TemperatureDissertation Submitted toTsinghua Universityin partial fulfillment of the requirementfor the degree ofDoctor of Natural SciencebyDong-ming YI( Physical Chemistry )Dissertation Supervisor : Professor Yong-chang TANG Associate Supervisor : Professor Da-long WUApril, 2001中文摘要摘要论文采用共振多光子电离和Ion-dip两种检测手段对碱土金属单卤化物的里德堡态进行了实验研究。
主要成果是:⑴首次观测到中等有效主量子数的CaCl 预解离里德堡态:在n*=5-7区域内,有5个文献未报导过的2∑+实贯穿里德堡态,填补了CaCl分子此一区域里德堡态研究的空白,对CaCl里德堡态结构的完整分析和其电子态完整的图像的建立具有重要意义;⑵通过理论分析,论证了这些态是因为和一个2∑+连续态的相互作用而导致强烈的预解离。
由实验测定的预解离线宽拟合出45000-47500cm-1范围内的2∑+连续态势能曲线,它能很好地解释这些里德堡态的预解离行为;⑶还观测到若干转动常数值反常小的里德堡态,它们可能是实非贯穿里德堡态的片段。
The Thermodynamics of the Earths Atmosphere The Earth's atmosphere is a complex system that interacts with the planet's surface, oceans, and biosphere. The study of the thermodynamics of the atmosphere is essential in understanding the behavior of this system and how it affects our planet. Thermodynamics is the study of the relationships between heat, energy, and work. In the context of the Earth's atmosphere, thermodynamics helps us understand the processes that govern the movement of air, the formation of weather patterns, and the distribution of energy throughout the system.One of the key principles of thermodynamics is the conservation of energy. This principle states that energy cannot be created or destroyed; it can only be transferred or converted from one form to another. In the Earth's atmosphere, energy is transferred through a variety of processes, including radiation, conduction, and convection. Radiation is the transfer of energy through electromagnetic waves, such as those from the sun. Conduction is the transfer of energy through direct contact, such as when the ground heats the air above it. Convection is the transfer of energy through the movement of fluids, such as when warm air rises and cool air sinks.Another important principle of thermodynamics is the second law of thermodynamics, which states that the total entropy of a closed system always increases over time. Entropy is a measure of the disorder or randomness of a system. In the Earth's atmosphere, entropy increases as energy is transferred from one place to another. This means that the atmosphere tends towards a state of maximum disorder, which can lead to the formation of weather patterns and other complex phenomena.The thermodynamics of the Earth's atmosphere also plays a crucial role in the global climate system. The atmosphere acts as a greenhouse, trapping heat from the sun and regulating the temperature of the planet. This is known as the greenhouse effect, and it is essential for life on Earth. However, human activities such as the burning of fossil fuels have increased the concentration of greenhouse gases in the atmosphere, leading to an enhanced greenhouse effect and global warming. Understanding the thermodynamics ofthe atmosphere is therefore crucial in addressing the challenges of climate change and developing strategies to mitigate its impacts.From a human perspective, the thermodynamics of the Earth's atmosphere has a profound impact on our daily lives. Weather patterns such as hurricanes, tornadoes, and thunderstorms are all driven by the movement of air and the transfer of energy through the atmosphere. These phenomena can have devastating effects on communities, causing loss of life and property damage. Understanding the thermodynamics of the atmosphere can help us predict and prepare for these events, improving our ability to respond and recover from natural disasters.In conclusion, the study of the thermodynamics of the Earth's atmosphere is essential in understanding the behavior of this complex system and its impact on our planet. Through the principles of conservation of energy and the second law of thermodynamics, we can gain insights into the processes that govern the movement of air, the formation of weather patterns, and the distribution of energy throughout the system. From a human perspective, this knowledge is critical in predicting and preparing for natural disasters and addressing the challenges of climate change. As we continue to explore the mysteries of our planet's atmosphere, the principles of thermodynamics will undoubtedly play a central role in our understanding of this fascinating and complex system.。
CHAPTER14DIRECT CURRENT(DC)DISCHARGES 14.1QUALITATIVE CHARACTERISTICS OFGLOW DISCHARGESThe dc glow discharge has been historically important,both in applications of weakly ionized plasmas and in studying the properties of the plasma medium.A dc discharge has one obvious feature,its macroscopic time independence,that is simpler than rf discharges.However,the need for the current,which provides the power for the discharge,to be continuous through the dc sheath provides an additional complication to the operation.This complication is not present in rf or microwave discharges where displacement current provides current continuity through the sheath.To understand the glow discharge,we consider the usual con-figuration of a long glass cylinder with the positive anode at one end and a negative cathode at the other.Although not necessarily the configuration used in processing applications,it has the advantage of symmetry and has been well studied.The usual pressure range of operation is between10mTorr and10Torr.Typically,a few hundred volts between cathode and anode is required to maintain the discharge. The approximate characteristics of the discharge are shown in Figure14.1.It is clear from the many light and dark regions identified in Figure14.1a that the beha-vior is quite complicated.The length of the positive column region can be varied by changing the distance between electrodes at a constant pressure and approximately constant voltage drop,while the other regions maintain their lengths.It is therefore Principles of Plasma Discharges and Materials Processing,by M.A.Lieberman and A.J.Lichtenberg. ISBN0-471-72001-1Copyright#2005John Wiley&Sons,Inc.535apparent that the positive column can be analyzed per unit length,while the other features must be analyzed in their entirety.All of the regions are gas,pressure, and voltage dependent in their size and intensity,with some of the smaller features being essentially absent over various parameter ranges.We now describe qualitatively the essential operation of the various regions in maintaining the discharge.The treatment follows most closely that in Cobine (1958)where additional material and references can be found.Positive ColumnThe axially uniform plasma is maintained by the JÁE power integrated over the cross section,which balances the loss of energy per electron–ion pair created, which,in the axially uniform model,is assumed to be radial.The dynamics are very similar to that of the bulk rf discharge,with the power lost per electron–ion pair created going to excitation(the glow),ionization,electron–neutral elastic scat-tering energy losses,and kinetic energy of the electrons and ions striking the walls. The normal glow discharge tends to have a negative voltage–current characteristic (negative differential resistance(d V=d I)which is stabilized by an external resistor, which is varied to adjust the current to the desired value.The power balance deter-mines the(weak)axial Efield required to maintain the positive column.Once E isknown,the drift velocity of the electrons along the column can be found using the dc14.1QUALITATIVE CHARACTERISTICS OF GLOW DISCHARGES537 electron mobility and then,from J,the density can be determined.We use this prescription in Section14.2to calculate the characteristics of the positive column.Cathode SheathThis region,known also as the cathode fall or Crookes dark space,is the region over which most of the voltage drop occurs.The electrons,which carry most of the current in the positive column,are,of course,prevented from reaching the cathode.The massive ions,however,are incapable of carrying the full current. The discharge is maintained by secondary electrons produced at the cathode by the impact of the energetic ions.This process,which is incidental(although often important)in rf discharges,is essential for the operation of the dc discharge.The current is built up by ionization within the sheath,which is generated by the second-ary electrons accelerating in the large electricfields of this region.The electron density andflux grow exponentially from the cathode,with the exponent known as thefirst Townsend coefficient.This mechanism is important,not only for the steady-state discharge,but also for understanding the breakdown that initiates the discharge.In breakdown the entire region between the cathode and the anode par-ticipates in the process,which requires a much higher voltage and therefore leads to hysteresis in the voltage–current characteristic.We analyze this dynamics in Section14.3.Negative Glow and Faraday Dark SpaceThe exponentially increasing density of high-velocity electrons near the cathode leads rapidly to a bright cathode glow in which intense ionization and excitation occurs.The electricfield must decrease rapidly at the end of this region,where the transition to the positive column occurs.However,the high electron velocities must be dissipated by elastic and inelastic collisions before the equilibrium conditions of the positive column can be established.This is done in a rather com-plicated process in which the electronsfirst lose almost all of their energy and then are reaccelerated in a weakfield over approximately a mean free path(the Faraday dark space).We give a simple approximate analysis of this behavior at the end of Section14.3.Anode FallThe drift velocity of the electrons in the weak electricfield of the positive column is typically less than their thermal velocity.This requires a retarding electricfield in the neighborhood of the anode to prevent the full thermal electron current from reaching the anode.However,the anode itself must clearly be positive with respect to the positive column to maintain the current.The result is a double layer,which is also seen in various other types of discharges,for essentially the same reason.Since the total voltage drop in this region is small and plays little role in the overall dynamics,we will not analyze it quantitatively.538DIRECT CURRENT(DC)DISCHARGESOther EffectsThe various other regions indicated in Figure14.1are not of particular significance for an overall understanding of the discharge behavior.In addition to the axial variations there are,of course,radial variations.In a long cylindrical discharge, we shall obtain the usual Bessel function radial variation as part of our solution for the positive column given in Section14.2.We may assume qualitatively similar radial variations of density in other regions,but quantitative calculations are very difficult.Additional radial features exist,such as an incomplete coverage of the cathode surface by the discharge,as we discuss in Section14.3.In the previous discussion we have considered the typical characteristics in the normal glow,which occurs over a range of current densities,typically between 10À5and10À3A=cm2.Considering current density as the controlling variable,the voltage–current characteristic of a dc discharge is shown in Figure14.2.Theflat region with slightly negative slope d V=d I is that of the normal glow.From low currents,the region below I A is called a dark or Townsend discharge.The glow gradually builds up until a transition is reached,with hysteresis,entering the normal glow at a voltage V S.The voltage remains constant as the current increases until I B,at which point there is an increasing voltage–current characteristic called the abnormal glow.A further increase in current results in a rather abrupt transition at I C,again characterized by hysteresis,to a considerably lower voltage discharge known as an arc discharge.The voltage continues to decrease with increasing current,approaching an asymptote.For a typical pressure(say1Torr)and a typical discharge tube of a few centimeters cross section,the transitions might occur at I A%10À6A,I B%10À2A,and I C%10À1A,but these currents dependon various other factors such as gas and electrode surfaces.There areapplications Array FIGURE14.2.Typical voltage–current characteristic of a dc glow discharge.14.2ANALYSIS OF THE POSITIVE COLUMN539 of these various regions,particularly for high current arc discharges,which wedo not consider.The reader canfind further descriptions of the behavior and theapplications in various monographs,for example,in Cobine(1958)and in Roth(1994).In some pressure and voltage ranges there are also interesting time-varyingphenomena,such as moving transverse striations and longitudinalfilaments.Athigh pressures,arc spots can form at the cathode,which correspond to an entirelydifferent range of operation,not considered here,in which the secondary emissionprocess is thermionic.For further study,the interested reader is referred to the litera-ture(Cobine,1958;Franklin,1976;Raizer,1991;Roth,1994).Sputtering and Other ConfigurationsA phenomenon that is not part of the discharge dynamics,but is important bothfor applications and in limiting the use of glow discharges,is cathode sputtering.The potential drop across a cathode sheath is typically several hundred volts.These ion-bombarding voltages lead to severe sputtering of the cathode surfaceand consequently deposit material on other surfaces.We describe physical sput-tering in Section9.3and its application to the deposition of thinfilms in Section16.3.Since there is little control over the large voltage drop in the cathodesheath,the existence of sputtering is important in defining appropriate appli-cations.Low aspect ratio dc discharges have been used for sputtering.Toenhance sputtering efficiency,other configurations of dc discharges have beenemployed.One configuration that has proved to be important for optical radiationsources and for metal-ion lasers is hollow cathode discharges.We treat this con-figuration in Section14.4.Another method of enhancing sputtering,used primar-ily for depositing metallicfilms on substrates,employs a nonuniform dc magneticfield.This configuration is called a dc planar magnetron discharge and is ana-lyzed in Section14.5.14.2ANALYSIS OF THE POSITIVE COLUMNAs in the analysis of rf and microwave discharges,there are various pressureregimes for which different dynamics apply.We will assume the following:(1)The pressure is sufficiently high,l i(T i=T e)R,that a diffusion equation with a constant diffusion coefficient D a applies.The low-pressure(collisionless)limit with freely falling ions,l i&R,was described very early by Tonks and Langmuir(1929);and the intermediate pressure regime,R!l i!(T i=T e)R,is discussed in Godyak(1986).In fact,as described in Section5.3,the radial dis-tributions in the low and intermediate regimes tend to look quite similar.Franklin (1976)describes these various solutions and relations between them.(2)As dis-cussed in Section14.1it is often adequate to assume only radial variation,which we do here.Calculation of T eThe calculation of T e follows from the particle balance as described in Section10.2. Ion particle balance is obtained from the diffusion equation(5.2.21)ÀrÁD a r n¼n iz n(14:2:1) where n¼n e¼n i is the plasma density,D a is the ambipolar diffusion coefficient, and n iz¼K iz n g is the ionization rate as defined in(3.5.1).In cylindrical coordinates (14.2.1)becomesd2n d r2þ1rd nd rþn izD an¼0(14:2:2)Equation(14.2.2)is Bessel’s equation with solution given by(5.2.35)n¼n0J0(b r)(14:2:3) where b¼(n iz=D a)1=2and J0is the usual zero-order Bessel function.If the ion mean free path l i and the sheath thickness s(s%few l De)are both small compared to the column radius R,then the boundary condition n(R)%0can be used,with the solution approximately given by(5.2.36)b¼n izD a1=2¼x01R(14:2:4)where x01%2:405is thefirst zero of the zero-order Bessel function.Although (14.2.4)does not give a completely self-consistent solution,since thefinite ion flux at the wall implies infinite velocity at zero density(see Section5.2),it can give a reasonably accurate value of T e.The reason is that n iz is a very sensitive func-tion of T e of the form(see Chapter3)n iz/p expÀE iz T e(14:2:5) with p the pressure and with the ionization voltage E iz)T e.Thus,T e depends only weakly on all parameters except for E iz.A more accurate solution is obtained by setting the radial particleflux G r equal to n s u B,where,as previously,n s is the density at the sheath edge and u B¼(e T e=M)1=2is the Bohm velocity.For this case,since G r¼ÀD a d n=d r,we can take a derivative of(14.2.3)to obtain a transcendental equation for the electron and ionflux to the wall(see also Section10.2):À(D a n iz)1=2J1(b R)¼J0(b R)u B(14:2:6) 540DIRECT CURRENT(DC)DISCHARGESBecause l i(R for this constant D a solution,(14.2.6)essentially reduces to(14.2.4).In the intermediate-and low-pressure regimes,l i&(T i=T e)R,the radial profile becomes relatively uniform,and the estimate for n iz(5.3.14)applies,n iz%2:2u BR4þRl iÀ1=2(14:2:7)An additional issue at low pressures is the deviation of the electron distribution froma Maxwellian.In using(14.2.5)we have assumed a Maxwellian,thus ignoring theelectron drift motion u e.This motion can readily be included(see Franklin,1976);with u e((e T e=m)1=2this does not appreciably change the results.More important, particularly at low densities,there are various kinetic effects and particle losses,thatcan affect the distribution at high velocities.We discuss these qualitatively at the endof this section.Calculation of E and n0The electricfield E along the z axis(anode-to-cathode)of the discharge is calculatedby equating the input power absorbed to the power lost.In the rf discharge this wasused to determine the density.Here the density cancels,leaving an expression for theelectricfield.However,once thefield is known,a subsidiary condition immediatelygives the density.Equating the ohmic power absorbedP abs¼2p ðRJÁE r d r(14:2:8)to the power lostP loss¼2p R G r e E T(14:2:9) where e E T is the total energy lost per electron–ion pair created,and substituting our radial density solution(14.2.3),we haveen0m e E22p ðRJ0(b r)r d r¼2p R(D a n iz)1=2n0J1(b R)e E T(14:2:10)where we have assumed a constant mobility m e,substituted for the current density J along z usingJ¼en m e E(14:2:11) and have taken E out of the integral by assuming that it is a constant in the long thin approximation.We see that n0cancels from(14.2.10)giving an equation for E14.2ANALYSIS OF THE POSITIVE COLUMN541alone.Performing the integration we find that J 1cancels,and we can solve for E to obtainE ¼n iz E T m e 1=2(14:2:12)Substituting m e ¼e =m n m ,from (5.1.4),then (14.2.12)can also be written in the formE ¼m e n iz n m E T 1=2(14:2:13)We note that n iz and n m are both linearly dependent on pressure,and that the only other dependence on the RHS is T e .Although (14.2.12)gives E as a function of p and as an exponentially sensitive function of T e through its dependence on n iz ,we can eliminate n iz using (14.2.4)to obtainE ¼x 01R D a E T m e 1=2¼x 01R mK m MK mi T e E T 1=2(14:2:14)which shows that E depends only on T e ,independent of p .Integrating (14.2.11)over the discharge cross section yieldsI ¼2p en 0R 2x 01J 1(x 01)m e E (14:2:15)which can be solved to determine n 0for a given discharge current I ,with E given by (14.2.14).Kinetic EffectsAlthough the preceding subsections give a qualitative description of the positive column,various quantitative discrepancies,particularly at lower pressures,have led to more sophisticated treatments.Particular phenomena to be explained are significantly higher average temperatures than predicted from (14.2.7)(with n iz cal-culated for a Maxwellian distribution),higher average energies near the column edge,an excess of local ohmic heating near the column edge compared to the local power dissipated in collisional processes,and a somewhat higher axial electric field.A full kinetic theory including the radial density variation is very complicated,so that various approximate kinetic methods have been employed.One important method is the nonlocal approximation,which we describe in Chapter 18.The basic idea is that,if the pressure is sufficiently low that l E =R .1,where l E isthe electron energy relaxation length,then the total energy e E ¼12m v 2þe F (r )542DIRECT CURRENT (DC)DISCHARGES14.3ANALYSIS OF THE CATHODE REGION543 can be taken to be a constant.For a Maxwellian electron distribution the conserva-tion of total energy is equivalent to the Boltzmann assumption that the temperature is constant and the potential and density are related in the usual logarithmic manner F(r)¼T e ln n(r)=n(0)ðÞ,with F(0)¼0at the plasma center.In this case a local macroscopic theory applies,as it does at high pressure for any distribution. However,we will see in Chapter18that the electron distribution in the positive column tends to be Druyvesteyn-like,falling more rapidly at high energies than a Maxwellian,with the high-energy electrons further truncated by the inelastic processes.Because of the non-Maxwellian distribution the average energy is significantly higher near the plasma edge than in the discharge center,since the lower energy electrons are confined by the potential,while the higher energy electrons can over-come the potential hill.The average energy is significantly higher than predicted by a Maxwellian because overall there are fewer high energy(ionizing)electrons. These effects have been confirmed by comparison with a more complete kinetic theory by Busch and Kortshagen(1995).Because the nonlocal method is limited to low pressures,other methods valid at higher pressure have been proposed(see Ingold,1997for another method of analysis and comparison among various methods).14.3ANALYSIS OF THE CATHODE REGIONConsidering the analysis of the previous section,we take as an example an argon glow discharge at p¼100mTorr and T e¼4V.The current density carried by the electrons in the glow is calculated from(14.2.11)J(r)¼en(r)m e Ewith m e%103m2=(V s)and E¼60V=m.Continuity of current requires the same current at the edge of the cathode sheath region,where the current is carried only by the ions.This can be approximated byJ i(r)¼en s(r)u Bwhere for argon at T e¼4V we calculate u B¼(e T e=M)1=2%3Â103m=s.This is considerably less than the electron drift velocity j u e j¼m e E¼6Â104m=s,and thus,even ignoring the difference between n s and n,it is not possible for the ions to carry the current in the cathode sheath.The resolution of this contradiction is that secondary electrons,created by ion impact at the cathode,are required to sustain the discharge.The process is similar to that involved in vacuum breakdown, and wasfirst analyzed in that context.Wefirst consider the more straightforward case of vacuum breakdown and then discuss the modifications required to treat the cathode sheath.Vacuum BreakdownConsider electrons emitted from a cathode at z ¼0being accelerated by an electric field and ionizing a neutral background.For a flux G e in the z direction (the direction of the field)a differential equation for the increase in flux can be writtend Ge ¼a (z )G e d z(14:3:1)with the solutionG e (z )¼G e (0)exp ðz0a (z 0)d z 0 !(14:3:2)where a (z );1=l iz (z )is the inverse of an “ionization”mean free path,analogous to the collisional mean free path defined in a similar way in Section 3.1.By continuity of total charge (creation of equal numbers of electron–ion pairs)the electron flux leaving the sheath edge at z ¼d ,minus the electron flux emitted at z ¼0,must be equal to the ion flux striking the cathode at z ¼0,minus the ion flux that enters at z ¼d :G i (0)ÀG i (d )¼G e (0)exp ðd0a (z 0)d z 0 !À1&'(14:3:3)where we have substituted for G e (d )from (14.3.2).For breakdown,the discharge must be self-sustaining.That is,setting G e (0)¼g se G i (0)where g se is the secondary electron emission coefficient at the cathode z ¼0,then (14.3.3)must be satisfied with G i (d )¼0.Solving for the exponential,we obtainexpðd0a (z 0)d z 0 ¼1þ1g se (14:3:4)as the self-sustaining condition.For a vacuum region,E is a constant and the electron drift velocity j u e (z )j ¼m e E ¼const.Hence the electron energy is a constant,allowing us to set a ¼const in (14.3.4).Taking the logarithm of both sides,we havea d ¼ln 1þ1g se (14:3:5)the usual form for the breakdown condition of a dc discharge.The quantity a is known as the first Townsend coefficient .As might be expected from our knowledge of cross sections,a is a complicated function of the pressure and the accelerating field,which is very difficult to calculate.However,we might expect a to be 544DIRECT CURRENT (DC)DISCHARGESexpressed in the forma ¼const l e exp ÀE iz E l e(14:3:6)where l e is the mean free path for inelastic (mainly ionization)electron–neutralcollisions,E l e is a typical electron energy gain in the field between collisions,and E iz is an energy for ionization.Here E l e plays the role that T e plays in (14.2.5).Recognizing that l e /p À1,then (14.3.6)can be written in the forma p¼A exp ÀBp E(14:3:7)where A and B are determined experimentally and found to be roughly constantover a restricted range of E =p for any given gas.Some experimental values of a =n g versus E =n g are shown in Figure 14.3.Here the gas density n g (m À3)¼3:25Â1022p (Torr)at room temperature from (2.3.18).The quantity a =n g is a field-intensified ionization cross section.The reduced field E =n g is often specified in units of townsends (1Td ;10À21V m 2).Fitting the form (14.3.7)to data such as shown in Figure 14.3,the coefficients in Table 14.1are constructed.Combining (14.3.7)with (14.3.5),and setting the breakdown voltage V b ¼Ed ,we have the relationApd exp ÀBpd V b ¼ln 1þ1g se(14:3:8)E nnFIGURE 14.3.Field-intensified ionization cross section a =n g versus reduced field E =n g(1Td ;10À21V m 2)(data provided by Petrovic´and Maric ´,2004).14.3ANALYSIS OF THE CATHODE REGION545Solving (14.3.8)for V b ,we obtainV b ¼Bpd ln Apd Àln ln 1þ1=g seÀÁÂÃ(14:3:9)We see that the breakdown voltage is a function of the product pd .For large values of pd ,V b increases essentially linearly with pd .For small pd there is a limiting value of pd ¼A À1ln (1þ1=g se )below which breakdown cannot occur.The breakdown voltage is a minimum V min at some intermediate value pd ¼(pd )min .The curve V b (pd )is called the Paschen curve ,and is a function of the gas and weakly a function of the electrode material.Typical breakdown curves for plane-parallel electrodes are shown in Figure 14.4.As we shall see,the values of V min and (pd )min play an import-ant role in the more complicated problem of the cathode sheath.Cathode SheathWe now consider the cathode sheath region of a discharge for which the electric field,and consequently a ,is not a constant with position.For a large sheath multiplication,we can still take G i (d )¼0in (14.3.3).Taking the logarithm of (14.3.4)we haveðd0a (z )d z ¼ln 1þ1g se (14:3:10)An exact solution for a (z )would involve an integral equation for the field and bevery difficult to solve.A simpler alternative is to measure the electric field distri-bution,which then becomes a known variation in determining a (z ).Somewhat surprisingly (Cobine,1958),it is found that the matrix sheath (constant ion space charge density,see Section 6.3)well approximates the region,giving a linearTABLE 14.1.Constants of the Equation a /p 5A exp(2Bp /E )AB Range of E /p Gas (cm21Torr 21)(V cm21Torr21)(V cm 21Torr 21)He 2.87730–250Ne 4.4111100–400Ar 11.5176100–600Kr 15.6220100–1000Xe 24330200–800H 2 4.813615–600N 211.8325100–600O 2 6.519050–130CH 417300150–1000CF 41121325–200Source :Fits to data supplied by Petrovic´and Maric ´(2004).546DIRECT CURRENT (DC)DISCHARGESfield variationE%E01Àz d(14:3:11)with z¼0at the cathode and z¼d at the sheath edge.Substituting(14.3.11)in (14.3.7)we havea p ¼A expÀBpE0(1Àz=d)!(14:3:12)and substituting(14.3.12)in(14.3.10)we obtainðd0Ap expÀBpE0(1Àz=d)!d z¼ln1þ1gse(14:3:13) FIGURE14.4.Breakdown voltage for plane-parallel electrodes at208C:(a)noble gases;(b)molecular gases(data supplied by Petrovic´and Maric´,2004).14.3ANALYSIS OF THE CATHODE REGION547which can be evaluated to give E0as a function of d.Integrating E in(14.3.11)from 0to d,we can express E0in terms of the cathode sheath(cathode fall)voltage V c as E0¼2V c=d,which when substituted in(14.3.13)givesAB(pd)2 2V c S2V cBpd¼ln1þ1gse(14:3:14)whereS(z)¼ðzeÀ1=y d y(14:3:15)is a known tabulated integral.If one plots V c(pd)for a given gas(given A and B)and given electrode material(given g se)wefind,as expected,curves that have a minimum V c¼V cmin at some(pd)min.We might expect the discharge to adjust itself to this stable value of d,and this is indeed the case in the normal glow region(see Fig.14.2).Some values of the cathode fall voltage are given in Table14.2a,and some corresponding normal glow cathode fall thicknesses are given in Table14.2b.These values are similar to the values for breakdown.We have not quite reached the end of the story.It is also possible to eliminate d in favor of the current density and gain both new insight into the operation of the normal glow region and also understand the abnormal glow operation.The total current density at the cathode is given byJ(0)¼en i(0)v i(0)(1þg se)(14:3:16)TABLE14.2a.Normal Cathode Fall in VoltsCathode Air Ar H2He Hg N2Ne O2Al229100170140245180120311Ag280130216162318233150C240475Cu370130214177447208220Fe269165250150298215150290Hg142340226K18064945917068Mg22411915312518894310Na2001858017875Ni226131211158275197140Pb207124223177210172Pt277131276165340216152364Zn277119184143216354Source:After Cobine(1958).548DIRECT CURRENT(DC)DISCHARGESwhere n i is the ion density,v i is the ion velocity,and g se gives the fraction of the current due to secondary ing Poisson’s equation with the assumption of constant charge density,we can write en i in terms of the cathode fall potential en i (0)¼e 02V c =d 2.Similarly,assuming a collisional sheath,we have v i (0)¼m i 2V c =d ,where m i is the ion mobility.Substituting these values in (14.3.16)we obtainJ (0)¼4e 0m i V 2c (1þg se )d 3(14:3:17)from which we can eliminate d in favor of J (0).Hence we can determine a Paschen-type curve of V c versus J (0).This is shown in Figure 14.5in terms of normalized parameters.It is clear that with a fixed external voltage source V T and resistance R T ,the dashed curve is unstable,such that if J ¼I =A ,J min ,where A is the effective cathode area;that is,ifV T ÀV cminR T A,J min(14:3:18)then the cathode fall area will constrict to a smaller value.This is the normal glow region.On the other hand,forV T ÀV cminR T A.J min(14:3:19)the solution is stable,and V c will increase with increasing current density.It is this region that is called the abnormal glow ,but as we can see,it is just as normal as the normal glow.TABLE 14.2b.Normal Cathode Fall Thickness pd in Torr cm Cathode Air Ar H 2He Hg N 2Ne O 2Al 0.250.290.72 1.320.330.310.640.24C 0.90.69Cu 0.230.80.6Fe 0.520.330.9 1.300.340.420.720.31Hg 0.9Mg 0.61 1.450.350.25Ni 0.90.4Pb 0.84Pt1.0Source :After Cobine (1958).14.3ANALYSIS OF THE CATHODE REGION549。
The concept of environmental protection and the dream of a green future have become increasingly significant in todays world.As the human population grows and industrialization expands,the impact on our planet has become a pressing concern.Here are some key points that could be included in an essay about the journey towards an environmentally friendly and sustainable future.Introduction:The importance of environmental protection in the21st century.The dream of a green future and its significance for the survival of our planet.The Current State of the Environment:The effects of pollution on air,water,and soil.The loss of biodiversity and the extinction of species.The impact of climate change and global warming.The Role of Governments and International Agreements:The role of the Paris Agreement in combating climate change.National policies and regulations aimed at reducing emissions and promoting renewable energy.Individual and Community Actions:The power of individual choices in reducing waste,conserving energy,and supporting sustainable products.Community initiatives such as tree planting,recycling programs,and local cleanup events.Technological Innovations:The development of clean energy technologies like solar,wind,and hydroelectric power. Advances in electric vehicles and public transportation to reduce reliance on fossil fuels.Education and Awareness:The importance of environmental education in schools and communities.Public awareness campaigns and the role of media in promoting green values.Challenges and Solutions:The economic challenges of transitioning to a green economy.Innovative solutions and the need for international cooperation.The Future of Green Living:Visions of smart cities and sustainable urban planning.The integration of green spaces and ecofriendly infrastructure.Conclusion:The collective responsibility of every individual,community,and nation to protect the environment.The hope for a greener,cleaner,and more sustainable future for generations to come.Call to Action:Encouraging readers to take steps towards a more sustainable lifestyle.The potential for each person to contribute to the global effort for environmental protection.By focusing on these points,an essay can effectively convey the urgency and importance of the environmental protection and the dream of a green future.It can inspire readers to consider their own role in this journey and to take action towards a more sustainable world.。
a rXiv:as tr o-ph/991243v12Dec1999Thermal and Ionization Aspects of Flows from Hot Stars:Observations and Theory ASP Conference Series,Vol.XXX,YYYY Henny mers,and Arved Sapar,plex wind dynamics and ionization structure in symbiotic binaries Rolf Walder 1Institute of Astronomy,ETH Z¨u rich,Switzerland Doris Folini 2Seminar of Applied Mathematics,ETH Z¨u rich,Switzerland Abstract.Aspects of the wind-dynamics in symbiotic binaries,collid-ing winds and accretion,are reviewed.Inconsistencies between theory and observations of the hot star wind are discussed.If the hot star wind were governed by CAK theory,nearly all symbiotics would be colliding wind binaries.For the case of colliding winds,3D hydrodynamical simulations reveal that the matter distribution is spirally shaped.Shock confined high-density shells as well as huge voids are found even in the immediate neighborhood of the stars.Synthetic spectra computed on the basis of different 3D hydrodynamical models suggest observational discrimination between them to be possible.Colliding wind models also provide a link between symbiotics and planetary nebulae.Accretion during some time is a necessary condition for symbiotics to exist.However,there is no proof of whether currently accreting systems show the symbiotic phenomenon.Existing accretion models are inconsistent amongst each other,predicting either extended disks or small,high-density accretion wakes.Synthetic spectra allowing to discriminate between two models do not yet exist.1.IntroductionSymbiotics have a complex dynamical behavior.Observations show variability on time scales of seconds to probably thousands of years.We know of bipolar outflows and jet-like features.Radio observations reveal complex and sometimes time-dependent structures of the circumstellar nebula.IR-emission often shows the presence of dust.From optical and UV spectra we take that the nebula has different velocity and density regimes.Many symbiotics are X-ray bright,revealing the presence of a hot (∼>107K)plasma.Some systems are quiet at the moment,from others we know that they underwent novae or smaller outbursts.Most of these phenomena are directly or indirectly related to the wind dy-namics of symbiotic systems.However,the very number of involved physical2Walder&Foliniprocesses and the large range of spatial and temporal scales prevented a con-sistent,quantitative model of symbiotics so far.But however,many successful attempts towards such a model.They form the basis of this review.In Section2 we discuss discrepancies between observations and CAK-theory for winds from the hot component.This question is decisive for whether symbiotics are collid-ing wind or accreting systems.In Section3,colliding wind models,their link to planetary nebulae,and their spectral response are presented.Accretion models are discussed in Section4.Finally,a summary is given in Section5.2.To what degree can photons from the hot primary drive matter? It is commonly accepted that the hot components in symbiotics are post AGB-stars which are reborn.There may be some exceptions,where the hot component is a neutron star or an accreting main sequence star.In this review,these exceptions as well as recurrent novae are explicitly excluded.For bringing back a white dwarf from its cooling track to a post AGB state accretion is an absolutely necessary condition.Accretion is also the basis for novae to occur and for shell-flashes proposed to explain symbiotic outbursts.On the other hand,we know of some symbiotics to be colliding wind systems.In this Section we discuss whether winds can be driven from the hot star and whether they can prevent accretion.M¨u rset et al.(1991)locate hot stars of symbiotics at the same place in the HR-diagram as central stars of planetary nebulae(CSPNe),when excluding the above mentioned exceptions.Hot primaries of symbiotics have temperatures above60’000K,many above100’000K,and luminosities between10and105L⊙with many of them around1000L⊙.Since CSPNe often loose mass,we expect fast,radiatively driven winds from the hot component in symbiotics as well. Theory For radiatively(line-)driven winds CAK theory predicts a momentum-luminosity relation(see e.g.Kudritzki1998)of˙Mv∞∝R−0.5∗L1/α∗[M∗(1−Γ)]3/2−1/α.(1)Γis the Eddington factor.αreflects the distribution function of the oscillator strength of all lines involved in the wind driving.Of course,αis a key parameter. In many cases,it is close to2/3,suggesting that the expression in the square brackets has potentially no influence.As we will see,more attention should be paid to the evaluation of photon-matter interaction for the case of symbiotics. Observations Comparing with observations(however,with not too hot stars with radii bigger than0.5R⊙),Kudritzki(1998)suggests thefits˙Mv∞=10AComplex wind dynamics and ionization structure in symbiotic binaries3 the limit with log r>−0.5was substantially higher.Based on HST/GHRS observation of the CIV155.0nm doublet,Patriarchi&Perinotto(1996)reportthat K1-16has a wind with3800km/s and a mass loss rate as low as˙M< 2·10−11M⊙/y.So far,this is one of the fastest winds of CSPNe ever measured.Symbiotics As long as the stars are not too hot,CAK-theoryfits well withthe observed evolution of winds after the outburst of symbiotic novae(Vogel&Nussbaumer1994;Schmid,this volume).But there are severe discrepancies between CAK-theory and observations for systems having a small,hot primary.For most symbiotics we have no observational evidence for a wind fromthe hot primary;see e.g.Dumm et al.(2000)for a discussion of the case ofRW Hya.In AG Peg,Nussbaumer,Schmutz,&Vogel(1995)observe P-Cygniprofiles indicating a wind with900km/s.Schmutz(1996)derives from spectra taken in1970R∗=0.5R⊙,L=1600L⊙,v∞=700km/s,˙M=10−6.7M⊙/y.For spectra taken in1994he derives R∗=0.06R⊙,L∼>500L⊙,v∞=950km/s,˙M=10−6.7M⊙/y.From a theoretical point of view,it is hard to understand whythe mass loss and the velocity from a shrinking star with decreasing luminositystay constant.According to CAK-theory(B=3,A=20,x=1.5),the wind parameters corresponding to the same temperatures and luminosities would bev∞=1700km/s,˙M=8.4·10−10M⊙/y(1970)and v∞=4900km/s,˙M=1.5·10−10M⊙/y(1994).Similarly in EG And.Vogel(1993)derives v∞=500km/sand˙M=2·10−9M⊙/y.The CAK-values corresponding to T∗=70′000K andL∗=15L⊙(M¨u rset et al.1991)are7000km/s and˙M=10−13M⊙/y.Thus,either luminosities and temperatures,or wind velocities and massloss rates derived from observations are wrong,or CAK-theory breaks downfor the winds from primaries in symbiotics.One systematic problem in the derivation of luminosities and temperatures by M¨u rset et al.(1991)and of the mass loss rate in EG And by Vogel(1993)is that a spherically symmetric mass distribution around the red star is assumed.Both,colliding wind and accretion models,however,predict that this is by far not the case.With regard to CAK, Springmann&Pauldrach(1992)note that in very rarefied winds the metals decouple from the bulk of the mass.This may lead to a much lower outflow velocity or even to a fall-back of hydrogen and helium.Porter&Skouza(1999), Porter(this volume),and Krti˘c ka&Kub´a t(this volume)discuss the idea in more detail.From the investigation of Gayley(1995)follows that stars withlow Eddington-factors(∼<5·10−4)are no longer able to drive winds1.However, most of the nowadays accepted values for symbiotics lie above this limit.Colliding wind models against accretion models Let us assume for a momentthat relation2is indeed valid for winds from the hot component in symbiotics. Then,assuming typical RGB-or AGB-winds respectively,it can be estimatedthat all systems with hot components having luminosities above10L⊙are col-liding wind systems.Even with very low mass loss rates,high speed winds have enough momentum to prevent circumstellar matter from falling onto the star.The question remains open whether this is true.4Walder&Folini3.Colliding windsThree dimensional computer models for colliding winds,even for comparatively simple physics,are still very demanding and need a lot of computer time.For symbiotics,only a very few have been presented,to our knowledge all by the Z¨u rich group(Nussbaumer&Walder1993,Walder1995a,Walder1995b,Walder 1998).We briefly review their results and add new ones from work in progress.3.1.Hydrodynamics:Carving,shaping and pushingWe discuss colliding winds at the example of three different3D hydrodynamical models.In all models,typical for S-type symbiotics,we assume an orbital period of two years,1.4M⊙for the cool and0.6M⊙for the hot star,20km/s for the cool star wind and1000km/s for the hot star wind.The three models differ in the mass loss rates for which we adopt˙M c=3.14×10−7M⊙/y,˙M h= 1.×10−9M⊙/y(model weak),˙M c=1×10−7M⊙/y,˙M h=2×10−9M⊙/y(model medium),and˙M c=3.14×10−8M⊙/y,˙M h=4×10−9M⊙/y(model strong). Consequently,the ratio of the momentumflux of the fast wind to that of the slow wind ranges from1/6(weak),over1(medium),to6(strong).For simplicity, we assume that both winds have reached their terminal velocity,and we neglect radiative forces and gravity.This assumption is critical for close systems where the wind-wind interaction zone and even the hot component itself may be located well within the acceleration region of the wind from the red star.Rotation of the stars is also neglected,which is another critical assumption,in particular for AGB stars.As the hot star works its way through the red giant wind,its own wind pushes material aside,leaving behind a spirally shaped,low density cavity.In the orbital plane as shown in Figure1,its role as a rotating snow-plow becomes particularly apparent.The opening angle of the spiral depends on the ratio of the momentumfluxes and is small in model weak and large in model strong.Matter is piled up at the leading edge of the spiral,where a shock bounded high density shell confines the interaction zone(starting in the upper half in the pictures). The trailing edge of the spirally shaped interaction zone is characterized by a huge rarefaction wave,connecting the high-density red star wind with the low density cavity of the fast wind in a smooth,however steep way.As the temperature is approximately constant across this trailing edge,the red-giant wind is re-accelerated by the resulting pressure-gradient.The models,therefore, predict a significant part of the red star wind to be faster than single star winds. The leading and trailing part of the interaction zone are connected by a small zone in the center where the two winds collide head-on.Looking now at the lower row of Figure1we notice in models weak and medium that the low-density spirally shaped tube carved by the hot star grows in diameter with increasing distance.The tube is eventuallyfilled again when the kinetic pressure of the fast wind is exhausted.However,this will happen on a scale significantly larger than our computational box of1·1015cm cubed.In both models the fast wind is embedded in the red giant wind material.In model strong the situation is different.Here the red star wind is basically restricted to a wide,open,high-density spiral.Normal to the orbital plane,the dense red giant wind is pushed away by the fast wind(see Section3.2.).Complex wind dynamics and ionization structure in symbiotic binaries5Figure1.3D Density(logarithmically labeled)and projected veloc-ityfield(v max=1000km/s)of the circumstellar matter for modelsweak(left),medium(middle)and strong(right).Top:slices alongthe orbital plane.The stars,rotating counterclockwise,are at the tipof the low-density cavity(hot)and in the center of the high-densityregion(cool).Bottom:slices normal to the orbital plane and along aline connecting the two stars.The stellar separation is3×1013cm,thecomputational domain1·1015cm cubed.We conclude that colliding winds force an extreme re-shaping of the cir-cumstellar material.The red star wind is no longer spherically symmetric,noris it smooth.Both,thin high density shells and huge voids can be found evenin the immediate neighborhood of the stars.Finally,we note that the interaction zone of the colliding winds is inherently unstable.High density knots andfilaments are formed.For a further discussionwe refer to our contribution on colliding winds in WR+O binaries(this volume), Walder&Folini(1998a),and the recent review of Walder&Folini(1998b). Additionally,instabilities induced by ionization may play an important role in symbiotics(e.g.Garc´ıa-Segura et al.1999).3.2.The planetary nebulae linkA common,bipolar,morphology and a similar dynamical behavior suggest alink between some D-type symbiotics and planetary nebulae.We want to makeonly two remarks here on this important link and refer to the review of Corradi (this volume)comprehensive discussion.6Walder&FoliniThe models discussed in Section3.1.show that the hot wind is confined by the dense wind from the red star whenever its momentumflux is comparable to or weaker than that of the cold wind.According to our simulations,the circum-stellar material should be strongly structured up to about1016cm.However, since the low-density voids occupy only a small volume,ionizing photons are unlikely to penetrate that far and no large-scale optical nebula will be present. But such a scenario may explain the radio measurements,e.g.of AG Peg by Kenny et al.(1991).On the other hand,if the momentumflux of the fast wind is bigger,all material is blown away in direction normal to the orbital plane, whereas in the orbital plane the presence of the red star prevents an unhindered outflow.A bipolar-like structure is likely to extend to scales similar to those of planetary nebulae.But even for a smaller momentumflux of the fast wind a bipolar large-scale structure may form if the circumstellar matter is more con-centrated in the orbital plane,e.g.due to accretion before outburst or due to rotation of the red star.Due to previous or currently on-going wind accretion,symbiotic hot stars have a good chance to be fast rotators and thus carry a larger magneticfield than single white dwarfs.Thus,a new class of magnetic wind models developed for planetary nebula may be of interest for symbiotics.These models show (Chevalier&Luo1994;Rozyczka&Franco1996;Garc´ıa-Segura1997)that rotating,magnetic CSPNe withfields of some hundred Gauss can explain the observed variety of shapes of planetary nebulae.In particular,elliptical and even bipolar nebulae form quite naturally.In addition,due to magnetic stresses, highly collimated jets can be formed(Garc´ıa-Segura et al.1999).These jets have a very particular velocity law,where the velocity is approximately linearly increasing along the jet-axis.Exactly such a law was observed in the young planetary nebulae MyCn18(Bryce et al.1997).These results prove that the presence of jets in a binary system does not require accretion.3.3.Spectral responseSpectra remain the main source of information on symbiotics although imaging is becoming more and more important with the new generation of telescopes. Due to the work of Corradi and Schwarz(e.g.Corradi&Schwarz1993),we have fantastic images of the large scale structure of D-type symbiotics.Radio images have also brought light into nebular substructures of some S-type symbiotics.There is a long tradition of applying photo-ionization codes to symbiotic sys-tems.Beginning with spherical symmetry(e.g.Nussbaumer and Schild1981), the models later were extended to axial-symmetry,where the hot star as the ionizing source illuminates the spherically symmetric wind from the cool star (e.g.Nussbaumer&Vogel1989;Proga,Kenyon,&Raymond1998).Below we report onfirst attempts where synthetic spectra are computed on the basis of 2D and3D hydrodynamical models,and thus include the influence of shocks, the wind-wind interaction zone,and the orbital motion.Optical and UV Based on axi-symmetric hydrodynamical models,Nussbaumer &Walder(1993)investigated the influence of the wind-wind interaction zone on the ionization structure and the spectrum of the symbiotic nebula.Remark-ably,the low-density cavity of the fast wind as well as the high-density wallsComplex wind dynamics and ionization structure in symbiotic binaries7Figure2.Phase-dependence of synthetic line profile for[O iii]λ5008for the models weak(left),medium(middle),and strong(right)with ahot star of100L⊙and90’000K.Profiles are computed for an observerin the orbital plane,phases are increasing from bottom to top,startingat phase zero(eclipse of hot star).Each line profile is plotted againstvelocity in km/s,negative velocities corresponding to motion towardsthe observer.of the wind-wind-interaction zone are as important as the luminosity and the temperature of the ionizing source.In particular,the high-density shells of the interaction zone can block high energy UV-photons,significantly reducing the emission area of highly ionized species.Velocities in these shells are significantly higher than red star wind pared to spectra computed from a single wind model,synthetic line profiles based on colliding wind models show significantly broader feet.Lines of highly ionized species are generally broaderthan lines of lower ionized species.In addition,the line-shapes significantly depend on the line of sight leading,suggesting that we should have a strong variation of the profiles over an orbit of the system.This was confirmed by the work of Folini(1998)who computed orbital variations of synthetic line profiles on the basis of the hydrodynamical models presented in Section3.1.It was also shown there that the line profiles as a wholeare shifted as a function of orbit.Moreover,it was demonstrated(see Figure2)that the same line([O iii]λ5008)computed for the same ionizing source(100L⊙and90’000K)may be shifted completely differently in each of the three models.If the line emission stems primarily from the immediate vicinity of thecool companion the line profile shows a maximum blue shift around phase0.On the other hand,if the emission stems from the interaction zone,maximumblue shift is reached around phase0.5.It was further shown that for each of the investigated models and ionizing sources it is possible tofind ions probing the interaction zone.X-ray emission Observed strong X-ray emission stood at the beginning of col-liding wind models of symbiotics.For the symbiotic novae HM Sge Kwok& Purton(1979)suggested a model where a shocked fast wind from the hot star leads to a spherical hot bubble.In contrast,Wallerstein et al.(1984)and Willson et al.(1984)suggested the observed X-rays to come from the head-on collision of the fast wind from the hot star with the slow,dense wind from thered star.Present models discussed in Section3.1suggest something in between.8Walder&FoliniThe collision zone of the two winds,and therefore the distribution of the hot plasma,is spirally shaped.Additionally,the hot star is expected to contribute with a supersoft component to the X-ray spectrum.First computational models of such two-component spectra were published by Walder&Vogel(1993)and M¨u rset,Jordan&Walder(1995).Observations:In a systematic study of16symbiotics M¨u rset,Wolff,& Jordan(1997)detected60percent of them as X-ray sources.All of them but two accreting neutron stars have a supersoft component.Seven show emission of an optically thin plasma with temperatures between3-20million Kelvins and the authors suggest an observational relation of L hot plasma=10−5L⊙.Theory:The case of a spirally shaped interaction zone described in Sec-tion3.1causes the entire fast wind to become shocked,at least for cases where the momentumflux of the red star wind dominates that of the fast wind.The resulting X-ray luminosity can be estimated as≈x eff×10−5(L∗/L⊙)1.5L⊙,(3) L xray=x eff×L mech CAKwhere the efficiency factor x eff lies between one and ten percent,depending on model parameters.So L xray is for luminous stars probably higher than the observed L hot plasma but the observational error bars are still large and in the theoretical prediction for L xray circumstellar absorption has been neglected. Concerning temperatures,the highest temperatures are reached in the system center where theflows collide head on.However,the bulk of the fast wind hits the spiraling interaction zone at angles much smaller than90degrees and the temperatures reached are smaller.Discussion:Assuming a colliding wind scenario,the X-ray emission is closely linked to the wind parameters.However,X-ray observations of EG And and AG Peg seem inconsistent with their wind parameters derived from obser-vations.CAKfit badly as well,but here the situation may be saved.Using a one temperaturefit to the observed X-ray spectrum M¨u rset et al. (1997)find1.5·107K for EG And.The wind parameters derived by Vogel (1993)lead to a theoretical peak temperature of only5.6·106K,CAK-based wind parameters result in unrealistic1.5·109K.Nevertheless,CAK-winds are not excluded by the observed X-ray spectrum of EG And for the following reasons. The bulk emission seen in X-rays is cooler than the theoretical peak temper-ature.Second,if heat conduction were taken into account peak temperatures would be generally reduced.As shown for hot star binaries by Myasnikov& Zhekov(1998)and by Motamen,Walder&Folini(1999)heat conduction be-comes important above about107K and will reduce the temperature by up to an order of magnitude.For AG Peg the situation is similar but less pronounced. From X-ray observations M¨u rset et al.(1997)derive3.16·106K.Observed wind velocities result in a peak temperature of1.5·107K,CAK based parameters lead to4·108K.While both sets of wind parameters seem possible,the CAK values may be preferable as again the X-ray observations reflect the bulk and not the peak temperature,and as heat conduction reduces peak temperatures.Finally, when taking observation based wind parameters the efficiency factor x eff must be below0.001tofit the observed X-rayflux.This is in contradiction with simulations.Moreover,CAK wind values result in x eff≈0.1,a value which is more realistic.Complex wind dynamics and ionization structure in symbiotic binaries9 4.AccretionAccording to current knowledge,the existence of every symbiotic system requires accretion at some stage.Yet,some symbiotics are observed to be colliding wind binaries.Is the observed symbiotic phenomenon compatible with accretion as well?The alternative would be that whenever accretion takes place the symbiotic signatures vanish.On observational grounds,this question has not been settled.And while colliding wind models are now compared to observations,accretion models are not yet sufficiently evolved.In the discussion below,most aspects are,however,of more general nature.Observations:Accretion sets free a relatively small amount of energy but various observational signatures may be explained in terms of accretion.As discussed by M¨u rset et al.(1991),observed UV nebular spectra from symbiotics require a more compact and hotter ionizing source than the emission from a classical Keplerian accretion disk.On the other hand,Sokoloski&Bildsten (1999)argue that the detected variation of1682seconds in the optical emission ofZ And may be explained by accretion onto a highly magnetic white dwarf.They attribute the outbursts to classical disk-instabilities of a Keplerian disk.Lookingat X-ray observations(temperature,luminosity,time variability),CH Cyg seemsto behave like a CV(Ezuka,Ishida&Makino1998,based on ASCA-spectra). However,according to M¨u rset et al.(1997)its X-ray properties are different fromany other symbiotic system,which all shows significantly lower temperaturesthat may be explained in terms of colliding winds.However,all these latter observations are ROSAT data only,therefore lacking a high-energy channel.The case of R W Hya:For RW Hya there are indications that it is a wind accreting system.If true,RW Hya is thefirst confirmed accreting symbiotic system.Dumm et al.(2000)discovered an unexpected occultation of the hot component at phaseφ=0.78.This occultation is unrelated to the eclipseof the hot component.The occultation lasts approximately∆φ=0.04.The spectral characteristics of this event indicate Rayleigh scattering due to a high column density of neutral hydrogen in the line of sight to the hot star.The authors interpret this observation in terms of an accretion wakefilled with highly compressed material,trailing the white dwarf.They corroborate this suggestionwith hydrodynamical simulations which show the formation of such a wake at approximately the correct orientation and opening angle.Theory:Wind accretion in separated but heavily interacting binaries with slow winds is not yet well understood.In S-type symbiotics Bondi-Hoyle-Lyttleton theory is not valid since here the Bondi accretion radius is compa-rable to the stellar separation.Walder(1997)reports that in such a situationonly6percent of the formal Bondi-Hoyle value can be accreted,correspond-ing,however,to6percent of the mass loss rate of the secondary.For binariesin which the Bondi accretion radius is small compared to the stellar separa-tion(e.g.HMXRB)63percent of the Bondi-Hoyle accretion rate is reached, corresponding,however,to only0.6percent of the mass loss rate of the sec-ondary.For D-type symbiotics,where the separation is a factor of10-20larger, Bondi-Hoyle-Lyttleton theory may be applicable but we are not aware of any simulations.Hydrodynamical studies of accreting systems with dynamical parameters comparable to S-type symbiotics were performed by Theuns&Jorissen(1993),10Walder&FoliniBisikalo et al.(1995,1996),Theuns,Boffin,&Jorissen(1996)and Mastrodemos &Morris(1998).Although there are significant differences between their results (see next paragraph)and despite their insufficient resolution close to the accret-ing star,all models agree on some issues:1)A large fraction of the donor-wind is captured by the accretor(up to10percent).2)In the vicinity of the accretor the density is strongly enhanced in the orbital plane and theflow spins.Some authors call this structure a disk.But even though theflow is spinning,it is still advection dominated and far from the regime of a viscous,Keplerian disk. Strong shocks are visible.3)There is spin up of the accreting star.4)All show complexly shaped nebulae on a scale of a few stellar separation.The wind from the red star is far from being spherically symmetric.The models,however,differ in one important aspect.According to Bisikalo et al.(1995,1996),a very extended(more than70R⊙!)disk is formed with no sign of a wake.All other results show a much smaller spinning structure with a very prominent wake trailing the accreting star.The main difference between these two simulation and all others is that Bisikalo et al.apply a Roche-potential based on both stars and neglect forces which accelerate the wind from the red star,whereas the other simulations all assume a net accelerating force(driving forces overwhelming gravity)from the donor star,together with gravitation from the accretor.None of the models considers radiative forces from the accreting star which,in fact,could be quite large as discussed in Section2.Bisikalo et al.(1996)provide synthetic Hβ-profiles on the basis of their2D hydrodynamical simulations.On top of a very broad foot–emitted by the disk –a thin nebular line can be found,varying in shape over an orbit.We know of no comparison of these profiles with observations.We conclude that accretion models predict a highly aspherical distribution of the circumstellar matter with a clear concentration in the orbital plane around the accreting star.Presumably,the disk-like structure is optically thick.Its spectrum can,however,probably not be compared with that of a Kepler disk since theflow is still advection dominated.5.SummaryTo explain the observed number of symbiotic systems,consisting of a hot post-AGB or pre-white dwarf and an evolved low-mass star,accretion must occur at some stage.So far,there is no direct observational proof that accretion takes place in any system we classify as symbiotic.For colliding winds,on the other hand,such evidence most likely exists for at least one system.In fact,the question whether accretion can occur at all in a system we observe as symbiotic is still under debate,as is the question of how the accretion takes place.A classic Keplerian disc is not mandatory.One of the key questions for both,colliding winds and accretion,is how the matter close to the white dwarf or in its atmosphere responds to the radiation field of this star.The overwhelming majority of symbiotics would have to be colliding wind systems if CAK theory were applicable for the wind of the white dwarf.However,there are inconsistencies between CAK-theory and observations which are not understood up to now.Likewise it has barely been investigated。