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crude treatment
相关语句
  原油处理
     Crude Treatment Integrating Design Technology
     原油处理一体化设计
短句来源
  “crude treatment”译为未确定词的双语例句
     The influence of structure of silicone surface active agents on behavior was reviewed. Their application in textile,detergent and cosmetics,ferment,coating and ink industry,and in polyurethane foamed plastics,fireextinguishing agent,emulsionbreaking and dehydrate of crude,treatment of powder were introduced.
     简述了有机硅表面活性剂的结构对性能的影响,并介绍了他们在纺织、日化、发酵、涂料和油墨工业以及在聚氨酯泡沫塑料、灭火剂、原油破乳、脱水、粉料处理等领域的应用。
短句来源
     Residue oil catalytic cracking is an important and major means in deep process in crude treatment.
     重油催化裂化是炼油厂重要的二次加工装置,是原油深度加工的重要手段之一。
短句来源
  相似匹配句对
     L. P. treatment.
     L. P.
短句来源
     Crude Treatment Integrating Design Technology
     原油处理一体化设计
短句来源
     Treatment of Acid Tar in Crude Benzene
     精苯酸焦油处理
短句来源
     Cough and Its Treatment
     咳嗽与咳嗽治疗
短句来源
     CRUDE WALLPAPER
     壁纸 让家离原野很近
短句来源
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  crude treatment
The elements of implantation are: combined external riser reactor; high-efficiency feedstock and slurry nozzles; crude treatment cyclone; cracking product cooling unit; two-stage catalyst stripping; regenerated catalyst transport system.
      
The need for using electric dehydrators in crude treatment plants
      
All flows were transferred by September 2001 and received crude treatment, secondary treatment was brought online in March 2002.
      


Basing on the character of fluting medium pulp which easily causes the producing of floating pulp、foam and floc. in the case of crude treatments in cleanimg and screen fractionation stages,we discussed pulp distribution、diffusing、 evening and mechanism of the Flowbox at the angle of fluid mechanics. Concluded that the headbox can aquire well distributed and stable diffused pulp flowing in a paper machine at the rate of 150m/min or so.

2400高强瓦楞原纸机流浆箱是根据瓦楞纸浆容易产生浮浆、泡沫及絮聚的流送特性,对其布浆、扩散、整流及结构从流体力学的角度进行了探讨,认为该流浆箱使用在抄速150m/min左右的纸机上,完全可以获得良好的、稳定的扩散浆流。

Ultraluminous IRAS galaxies (ULIRGs), characterized by their high far infrared luminosities L IR >10 12 L ⊙(for H 0=50 km s -1 Mpc -1 ), are among the most luminous galaxies in the local universe (see Sanders & Mirabel 1996 for a review). Most ULIRGs show signs of interaction and/or merging. These processes are believed to trigger starbursts and central nuclear activities that in turn produce intense infrared emissions via dust absorption and re emission. Some ULIRGs do not show prominent...

Ultraluminous IRAS galaxies (ULIRGs), characterized by their high far infrared luminosities L IR >10 12 L ⊙(for H 0=50 km s -1 Mpc -1 ), are among the most luminous galaxies in the local universe (see Sanders & Mirabel 1996 for a review). Most ULIRGs show signs of interaction and/or merging. These processes are believed to trigger starbursts and central nuclear activities that in turn produce intense infrared emissions via dust absorption and re emission. Some ULIRGs do not show prominent interaction signatures from ground based imaging, but high resolution HST observations revealed secondary nuclei at their centers and additional tidal features (Borne et al 1999). Also some of these ULIRGs could be advanced mergers, as is the case for the ULIRGs with highest luminosities (L IR >10 12 L ⊙,for H 0=75 km s -1 Mpc -1 ) (see, e.g., Sanders & Mirabel 1996). These ULIRGs may represent an important stage in formation of QSOs and powerful radio galaxies, and could be an essential step in the formation of elliptical galaxies (Sanders et al 1988a; Sanders & Mirabel 1996; Melnick & Mirabel 1990). Although the ultimate fate of the ULIRGs is not yet fully understood, more and more observations show that merger remnants resemble elliptical galaxies or S0 galaxies. For example, the surface brightness profile of IRAS 20551-4250 is reasonably well fitted by the R 1/4 law (Johansson 1991). Arp 220 and NGC 6240, two nearest ULIRGs, both have densities, velocity dispersions and central surface brightness distributions consistent with the fundamental plane of elliptical galaxies (Doyon et al 1994). Baker & Clements (1997) investigated the old stellar population for 10 nearby ULIRGs based on deep near infrared imaging and concluded that 8 out of 10 ULIRGs show signs of elliptical structure. On the theoretical side, Toomre & Toomre (1972) first successfully reproduced the observed bridges and tails using restricted three body simulations of two colliding disk galaxies. In 1977, Toomre put forward the hypothesis that all elliptical galaxies could be remnants of merged disk galaxies. Later simulations improved the spatial resolutions, explored more phase space of the encounter geometry and incorporated more realistic treatments of the progenitors, adding components such as bulges, massive dark matter haloes and gas; crude treatment of star formation is also attempted (e.g. White 1978; Farouki & Shapiro 1982; Negroponte & White 1983; Barnes 1992; Hernquist 1992; Heyl et al 1994; Barnes & Hernquist 1996; Weil & Hernquist 1996; Walker et al 1996; Mihos & Hernquist 1994). These simulations conclude that a wide range of initial conditions can result in the formation of early type like galaxies and the R 1/4 law (Lynden Bell 1967; see de Zeeuw & Franx 1991 for a review). Besides the global elliptical like characteristics of the remnants of simulated mergers (e.g. the r 1/4 law of the surface brightness profile), some simulations also attempt to reveal the fine structure of the remnants such as the shape of isophotes, loops, shells and tails (see e.g. Heyl et al 1994; Springel & White 1998). As mergers of galaxy pairs may not account for all observed properties of ellipticals, multiple mergers have also been considered (Mamon 1987, Barnes 1984, Barnes 1985, Barnes 1989, Schweizer 1989; Weil & Hernquist 1996); this may occur in compact groups such as those found by Hickson (1982, 1993).While the simulations indicate that merging of two or more disk galaxies can lead to the formation of ellipticals, it is clearly important to test these predictions empirically. The ULIRGs are ideal laboratory for this purpose, since they are closely related to galaxy merging and interactions (e.g., Murphy et al 1996, Clements et al 1996). We analyze the surface photometry for 13 ULIRGs observed with the Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC2) in the I band, and examine whether their profiles resemble the R 1/4 law, as one would expect if they ultimately form ellip

 星系间的相互作用和并合是一个非常普遍的现象, 在星系的形成和演化过程中扮演了一个重要角色。理论和实测都有表明星系并合是椭圆星系形成的重要途径。极亮红外星系(ULIRGs) 与星系间的相互作用和并合密切相关,是研究星系并合现象的理想实验室,对它们的测光研究将有助于理解星系的并合过程。哈勃望远镜(HST) 的高分辨率观测为这方面的研究提供了条件。我们利用哈勃望远镜(HST) 的宽场行星照相机( WFPC2) 对极亮红外星系短曝光巡天的I波段数据,选出了一个子样本。该子样本由21 个以单核为主的极亮红外星系组成,这些星系一般处于星系并合的晚期。我们对这些星系进行了面源测光研究,并根据面亮度轮廓与R1/4 律的差别利用χ2 判据律将它们分成了两大类:第一类八个星系的面亮度轮廓可以用R1/4律很好地拟合;而第二类星系在面亮度轮廓与R1/4 律差别较大。对测光行为的定性分析表明,第二类星系可以进一步分为两个子类:五个IIa 类星系和八个IIb 类星系。Ⅱa 类星系的面亮度轮廓由三部分组成:中心的亮核,内区可用R1/4 律描述的成分以及外面的延展部分。IIb 类星系的面亮度轮廓和R1/4 律有着不同程度的差异。我们还利用...

 星系间的相互作用和并合是一个非常普遍的现象, 在星系的形成和演化过程中扮演了一个重要角色。理论和实测都有表明星系并合是椭圆星系形成的重要途径。极亮红外星系(ULIRGs) 与星系间的相互作用和并合密切相关,是研究星系并合现象的理想实验室,对它们的测光研究将有助于理解星系的并合过程。哈勃望远镜(HST) 的高分辨率观测为这方面的研究提供了条件。我们利用哈勃望远镜(HST) 的宽场行星照相机( WFPC2) 对极亮红外星系短曝光巡天的I波段数据,选出了一个子样本。该子样本由21 个以单核为主的极亮红外星系组成,这些星系一般处于星系并合的晚期。我们对这些星系进行了面源测光研究,并根据面亮度轮廓与R1/4 律的差别利用χ2 判据律将它们分成了两大类:第一类八个星系的面亮度轮廓可以用R1/4律很好地拟合;而第二类星系在面亮度轮廓与R1/4 律差别较大。对测光行为的定性分析表明,第二类星系可以进一步分为两个子类:五个IIa 类星系和八个IIb 类星系。Ⅱa 类星系的面亮度轮廓由三部分组成:中心的亮核,内区可用R1/4 律描述的成分以及外面的延展部分。IIb 类星系的面亮度轮廓和R1/4 律有着不同程度的差异。我们还利用自己的观测和文?

Not only heparin hydration,resin absorption,elution,crude treatment but also ether the usage and treatment of resin D-254 were reported in this paper.The collecting ratios,12.1%,11.1%~19.2%,15.1% as well as 20.7%and4.4% were increasing in the processes of protease hydration,the second hydration,the second resin absorption as well as the second and the third elution of NaCl.While Na 2SO 4 and precipitate YNB 99-1 were utilized for conservation,the collectiong ratio of heparin activity was up to...

Not only heparin hydration,resin absorption,elution,crude treatment but also ether the usage and treatment of resin D-254 were reported in this paper.The collecting ratios,12.1%,11.1%~19.2%,15.1% as well as 20.7%and4.4% were increasing in the processes of protease hydration,the second hydration,the second resin absorption as well as the second and the third elution of NaCl.While Na 2SO 4 and precipitate YNB 99-1 were utilized for conservation,the collectiong ratio of heparin activity was up to 98.1% in HCl treatment which made heparin potency become to more than 90 USP u/mg.For guaranteeing the stability of heparin collectiong ratio,the quantity of used D-254 resin had to be increased month by month and treated with ethanol.

研究了提高肝素钠产率的主要工艺条件 ,肝素钠生产中 4种提高收率的方法结果表明 :(1)酶解提取比盐解增加收率 12 .1% ,酶、盐解二次提取提高 11.1%~ 19.2 % ;(2 )二次吸附提高收率 15.1% ;(3)二、三次洗脱分别增加 2 0 .7%和 4 .4 % ;(4 )粗产品精制处理。加入Na2 SO3和沉淀剂YNB 99- 1收率可达 98.1%。 1种稳定产率的措施是逐月增加树脂用量和添加乙醇再生处理树脂。

 
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