淀粉粘合剂生产与应用中的几个问题

本针对淀粉粘合剂生产和应用中存在的几个问题，从理论和实践上进行了探讨。这些问题包括氧化反应速度不稳定、纸板干燥速度、纸板挺度、粘合剂的储存稳定性。     

超焦距对焦法的理论修正和完善

通过严密的数学运算，从理论上对焦距对焦法作出了修正和完善，并探讨了这种修正和完善在摄影技术中的实际意义。     

人防地下室顶板加层设计

以某人防地下室顶板加层项目为实例，通过对结构进行分析计算，探讨了加层设计中应注意事项及计算方法，对类似工程有一定的参考价值.     

胆红素锶的EXAFS和FT—IR研究

以胆红素(H_2BR)为原料,合成组成为SrBR·2H_2O的胆红素锶,并进行了EXAFS研究,得知胆红素锶的第一配位层包含0和N两种原子,配位数为8,其Sr-O和Sr-N距离分别为2.60A和2.69A。比较H_2BR和SrBR·2H_2O的FT-IR光谱,根据-NH,-COOH和内酰胺等谱带变化,提供了胆红素中含氮和含氧基团与锶配位的证据,与EXAFS实验结果相互一致。     

Chaotic capture of Jupiter's Trojan asteroids in the early Solar System

Jupiter's Trojans are asteroids that follow essentially the same orbit as Jupiter, but lead or trail the planet by an angular distance of approximately 60 degrees (co-orbital motion). They are hypothesized to be planetesimals that formed near Jupiter and were captured onto their current orbits while Jupiter was growing, possibly with the help of gas drag and/or collisions. This idea, however, cannot explain some basic properties of the Trojan population, in particular its broad orbital inclination distribution, which ranges up to approximately 40 degrees (ref. 8). Here we show that the Trojans could have formed in more distant regions and been subsequently captured into co-orbital motion with Jupiter during the time when the giant planets migrated by removing neighbouring planetesimals. The capture was possible during a short period of time, just after Jupiter and Saturn crossed their mutual 1:2 resonance, when the dynamics of the Trojan region were completely chaotic. Our simulations of this process satisfactorily reproduce the orbital distribution of the Trojans and their total mass.     

Origin of the orbital architecture of the giant planets of the Solar System

Planetary formation theories suggest that the giant planets formed on circular and coplanar orbits. The eccentricities of Jupiter, Saturn and Uranus, however, reach values of 6 per cent, 9 per cent and 8 per cent, respectively. In addition, the inclinations of the orbital planes of Saturn, Uranus and Neptune take maximum values of approximately 2 degrees with respect to the mean orbital plane of Jupiter. Existing models for the excitation of the eccentricity of extrasolar giant planets have not been successfully applied to the Solar System. Here we show that a planetary system with initial quasi-circular, coplanar orbits would have evolved to the current orbital configuration, provided that Jupiter and Saturn crossed their 1:2 orbital resonance. We show that this resonance crossing could have occurred as the giant planets migrated owing to their interaction with a disk of planetesimals. Our model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations.     

α-烷基-β-(2,2,3-三甲基-3-环戊烯基)乙醇及烷基(2,2,3-三甲基-3-环戊烯基甲基)酮的合成

以α-藻烯为原料,经环氧化等一系列反应得到α-烷基-β-(2,2,3-三甲基-3-环戊烯基)乙醇和烷基(2,2,3-三甲基-3-环戊烯基甲基)酮(烷基分别为乙基、正丙基、异丙基、正丁基、异丁基、二级丁级、三级丁基、正戊基、异戊基、正己基、2-乙基丁基和环己基)共24个新化合物,并通过波谱及色谱确定了它们的结构及含量。     

天然海水中氨基酸复合缓蚀剂对黄铜缓蚀性能的研究

采用动电位极化和交流阻抗法测定海水环境中L-半胱氨酸及赖氨酸对黄铜试样的缓蚀性能，然后将这两种氨基酸分别与葡萄糖酸钠复配，研究其缓蚀协同作用。结果表明：单独使用L-半胱氨酸及赖氨酸，缓蚀效率最高分别为87.5%和89.93%；与葡萄糖酸钠复配后，两组复合缓蚀剂的缓蚀性能均显著提高，缓蚀效率分别达到97.35%和98.62%；两种氨基酸缓蚀剂在黄铜表面的吸附均遵从Langmuir吸附等温线。葡萄糖酸钠的加入弥补了单独使用氨基酸缓蚀剂吸附膜致密性差的缺陷，另外扫描电镜实验结果也显示缓蚀剂的加入明显抑制了金属的腐蚀。