Synthesis and Characterization of a Homochrial Manganese（Ⅱ）Complex Constructed from （1R,2R）-（-）-Diaminocyclohexane-N,N biscarboxyl-salicylidene）

A homochrial manganese(Ⅱ) complex derived from chiral salen ligand (1R,2R)-(-)diaminocyclohexane-N,N-biscarboxyl-salicylidene) (1) has been synthesized through solvothermal procedure and characterized by IR,elemental analysis,TGA,circular dichroism (CD),powder and single-crystal X-ray crystallography.It crystallizes in monoclinic,space group C2 with a=32.987(7),b=7.4662(15),c=17.931(4),β=97.82(3)°,V=4375.0(15) 3,Z=8,D c=1.544 g/cm 3,F(000)=2096,M r=508.36,μ=0.658 mm-1,the final GOOF=0.975,R=0.0676 and wR=0.2068 for 6357 observed reflections with I > 2σ(Ⅰ).The coordination polymer 1 possesses a 1D infinite zigzag chain architecture constructed by the dicarboxyl-functionalized metallosalen ligand (MnSalen),and the polymeric chains are further assembled into a 2D supramolecular network structure via strong intermolecular hydrogen bonding interactions between the adjacent zigzag chains.     

31.2MeVα粒子在10,11B核上散射的研究

我们测量了31.2MeV的α粒子对^10,11B的散射角分布,结果表明在¹⁰B核上有反常现象;在¹¹B则无反常现象。我们采用了光学模型加雷奇极模型进行了计算和分析,结果表明,对于1p壳核,诸如α+¹⁶O,计算结果与实验测量很好符合,而对于α+¹⁰B则不成功。采用双v次幂光学模型分析时,对于α+¹⁶O的符合程度稍次于前者的结果;对于α+¹⁰B仅能定性符合。众所周知,上述模型对于α+⁴⁰Ca的分析与实验结果的符合是十分好的。由此可以得出结论:2s-1d壳核与1p壳核的大角反常散射的机制不同;同时也表明1p壳核的反常散射机制亦有差异。     

裂解气相色谱-质谱法研究聚醚酰亚胺的热裂解行为

采用裂解气相色谱-质谱技术研究了聚醚酰亚胺(PEI)在550℃、650℃和750℃裂解温度下的热分解行为.随着裂解温度上升,裂解产物明显增加.在750℃时聚合物分子链断裂完全,共鉴别到25种碎片组分.PEI热分解的碎片中叔丁基苯酚、叔丁基甲基苯酚、苯酚、苯胺、氰苯、2-苯基-1H-异吲哚-1,3(2H)-二酮等5种裂解产物最重要,因此可以依据这几种化合物定性鉴别聚醚酰亚胺.依据热分解产物的数量以及结构推断降解机理为:裂解首先从醚键开始,其次是酰胺基团中的C-N键,然后再经过一系列消除反应、成环反应、重排反应等形成多种裂解碎片.     

氢氧化锰共沉淀分离-催化极谱法测定土壤中有效钼

土壤样品中有效钼用草酸铵-草酸混合溶液(pH 3.3)振摇提取,所得悬浮液用干滤纸过滤,分取部分滤液蒸缩体积后加入10 g.L-1酸性高锰酸钾溶液并蒸发至近干,趁热加0.25 mol.L-1氢氧化钠溶液进行共沉淀分离。分取部分上清液,用硫酸(1+1)溶液酸化后加入混合底液(其中含有二苯基乙醇酸、二苯胍及氯酸钠)及少许钛铁试剂溶液作为与钼(Ⅵ)进行催化反应的试剂体系。用JP-303极谱仪进行测定。在-220 mV峰电位处测得的峰电流值与其相应的钼(Ⅵ)的质量浓度在0.8～20μg.L-1范围内呈线性关系。此方法的检出限(3s/k)为0.002 6μg.g-1。用此方法分析了5个土壤标准物质,所测得有效钼的含量与其认定值相符。     

Charged vortex structure in high-temperature superconductors

By using a model Hamiltonian with competing antiferromagnetic (AFM) spin density wave (SDW) and d-wave superconductivity orders, the effect of next-nearest-neighbour (nnn) hopping on spin and charge structures in high-temperature superconductors is investigated at finite temperatures. For an optimally doped sample, we find that the AFM order magnitude in the vortex core is firstly enhanced and then suppressed, accompanied with a ``positively → negatively → positively" charged vortex structure transition with increasing nnn hopping strength, which implies that the AFM order is unnecessarily bounded to an electron-rich vortex core. In addition, a charge ordering pattern with four negatively charged peaks localized in a small region is also found around the vortex core centre without net charge. Recent scanning-tunneling-microscopy experimental observations of the checkerboard structure are hopefully understood.     

大口径毛细管柱气相色谱法直接测定工作场所空气中丙烯酰胺

以水为吸收液采集工作场所空气样品中的丙烯酰胺,采用大口径毛细管柱气相色谱法直接测定吸收液中丙烯酰胺的含量,采用HP-INNOWAX色谱柱(30m×0.53mm,1.00μm)分离,氢火焰离子化检测器检测。丙烯酰胺的质量浓度在0.050～3.00mg·L~(-1)内与其对应的峰面积呈线性关系,检出限(3S/N)为0.014mg·L~(-1)。对丙烯酰胺标准溶液进行测定,测定值的日内相对标准偏差(n=6)为1.0%～2.1%,日间相对标准偏差(n=6)为1.3%～2.2%。以空白样品为基体进行加标回收试验,所得回收率为93.0%～102%。     

Geometry and optics calibration of WFCTA prototype telescopes using star light

The Large High Altitude Air Shower Observatory (LHAASO) project is proposed to study high energy gamma ray astronomy (40 GeV--1 PeV) and cosmic ray physics (20 TeV--1 EeV). The wide field of view Cherenkov telescope array, as a component of the LHAASO project, will be used to study the energy spectrum and composition of cosmic rays by measuring the total Cherenkov light generated by air showers and the shower maximum depth. Two prototype telescopes have been in operation since 2008. The pointing accuracy of each telescope is crucial for the direction reconstruction of the primary particles. On the other hand, the primary energy reconstruction relies on the shape of the Cherenkov image on the camera and the unrecorded photons due to the imperfect connections between the photomultiplier tubes. UV bright stars are used as point-like objects to calibrate the pointing and to study the optical properties of the camera, the spot size and the fractions of unrecorded photons in the insensitive areas of the camera.