基于Ru（bpy）3^2＋印刷电极的电致化学发光传感器的研制

利用丝网印刷技术制备了基于Ru(bpy)23 (钌联吡啶)的印刷电极电致化学发光传感器,这种传感器具有制作简单、成本低、重现性好、对草酸盐的响应范围宽、检测限低等优点。详细研究了电极的制作方法以及发光试剂的固定化。在最优条件下,在pH 6.0的0.2 mol.L-1磷酸盐缓冲液中,利用所研制的ECL传感器测定C2O24-,线性响应范围为3.0×10-7~1.0×0-5mol.L-1,检测限为1.2×10-7mol.L-1(S/N=3)。根据同样的原理也可以用来测定其他的成分,如氨基酸,TprA(三丙胺),NAD(烟酰胺腺嘌呤二核苷酸)等物质。同时应该指出的是如果使用丝网印刷机器进行印刷的话,电极的重现性和稳定性还可以进一步提高。     

NCl（a^1△）／I（^2P3／2）传能体系的实验研究

利用微波放电C12／He等离子体作为Cl源，对反应NCl(a^1△) I(^2P3/2)→NCl(X^3∑) I(^2P3/2)进行了实验研究，得到了较大的I(^2P3/2)自发辐射荧光信号，检测到NCl(a^1△，b^1∑)自发辐射荧光光谱在存在少量I(^2P3/2)下发生的显著变化，其中NCl(a^1△)自发辐射荧光信号降低，同时由于I(^2P3/2)的作用，NCl(b^1∑)自发辐射荧光信号大幅度增加。在考察各反应气体流量对I(^2P3/2)自发辐射荧光信号的影响时发现，在本次实验条件下，各种气体的最佳流量：He为1—4mmol/s，I2为0．01—0．03mmol/s，Cl2为1．0mmol/s左右，而HN3流量略大于Cl2流量时信号升高幅度开始变缓，约为Cl2流量的两倍时信号不再有显著的变化。     

（XB2）2（X=Al，Be，Na，Mg）团簇结构与性质的密度泛函研究

用密度迁函理论（DFT）的杂化密度泛函B3LYP方法在6-31G＊基组水平上对（XB2）2（X=Al,Be，Na，Mg）团簇各种可能的构型进行几何结构优化，预测了各团簇的最稳定结构．并对最稳定结构的电子结构、振动特性、成键特性和电荷特性等进行了理论研究．结果表明，团簇的几何结构大多是平面结构，通常是B—B键和B—X键共存，较少出现X-X键，团簇的稳定结构中通常是几个呈负电性的B原子形成一个负电中心，而其他B原子和X原子处在端位，且显正电性。     

体光源模拟标定法测O2（^1△）绝对浓度

O2(^1△)绝对浓度的测量,一直是SOG和COIL研究中的重要参数之一。体光源模拟标定法测O2(^1△)绝对浓度,是把发光气体以某一流速引入一已知体积的流动光池中,再通过具有低象差失真的光学系统,把该体光源成象在探测器的有效表面上。探测器和测量仪器组成的测量系统,要经过标准光源和电学标定。本方法可测出O2(^1△)绝对浓度及其分压,O2(^1△)产率等参数。其中O2(^1△)浓度测量结果的相对误差为20％。     

Search for the Halo Effect in the ^1H（^6He,^6Li）n Reaction

The angular distributions of the charge exchange reaction ^1H(^6He,^6Li)n were measured in reverse kinematics with a secondary ^6He beam at the energy of 4.17 A MeV.The data were analysed in the context of a microscopic calculation.It is shown that both the ground state of ^6He and the second excited state of ^6Li(3.563MeV,0^ ) have a halo structure.     

新试剂1-（偶氮苯基）-3-（4,5-二甲氧基-2-苯甲酸）-三氮烯与铜（Ⅱ）的显色反应

研究了1-（偶氮苯基）-3-（4,5-二甲氧基-2-苯甲酸）-三氮烯（ABDMBAT）试剂与Cu（Ⅱ）的显色反应。在TritonX-100的存在下,pH 11.0的Na2B4O7-NaOH缓冲溶液中,该试剂与铜形成红色络合物,ABDMBAT与Cu（Ⅱ）形成的络合物的最大吸收峰位于540nm处,表观摩尔吸光系数ε=8.26×104L.mol-1.cm-1,Cu（Ⅱ）在0—14μg/25mL范围内服从比耳定律。     

（LiN3）n（n=1～2）团簇结构与性质的密度泛函研究

用密度泛函理论（DFT）的杂化密度泛函B3LYP方法在6—31G^＊基组水平上对（LiN3）n（n=1～2）团簇各种可能的构型进行几何结构优化，预测了各团簇的最稳定结构．并对最稳定结构的振动特性、成键特性和电荷布局等性质进行了理论研究．结果表明，LkN3团簇最稳定构型为直线构型；（LiN3）n（n=1～2）团簇中N—N键长在0．1146-0．1203nm之间，N—Li键长在0．1722～0．1987nm之间；团簇中Li原子全部显正电性，越靠近Li原子的N原子负电性越强，在直线构型的Nf离子中，两端的N原子均具负电荷，而中心N原子具正电荷．     

方列管型射流式O2（^1△）发生器的COIL出光研究

方列管型射流式O2(^1△)发生器是一种新型高效的氧碘化学激光器(COIL)化学能源供给装置。描述了采用该发生器在COIL上所做的一系列出光实验,这些实验着重于考察该发生器的性能参数及相应的COIL化学效率。结果在Cl2流量为0．25mol／s、无冷阱、稳定腔条件下获得化学效率高达26％。     

重金属钋化物分子MPo（^2Ⅱ），（M=Cu，Ag，Au）的结构和势能函数

利用相对论小核赝势研究了重金属钋化物分子MPo（X^2Ⅱ），（M=Cu，Ag，Au）．用群论方法结合原子分子反应静力学原理导出了分子的基电子状态和相应的离解极限，并在各种电子相关理论水平上计算了它们的平衡几何和振动频率．在此基础上用Murrell—Sorbie函数形式拟和势能曲线，得到了总的解析势能函数，并计算出了光谱数据和力常数．     

CS2分子^1B2（^1∑u^＋）态预解离动力学研究

研究了CS2分子^1B2(^1∑u^+)预离解态线形势垒下的g振动能级光解动力学，包括预解离寿命、产物振转布居、平动-振动-转动能量分配和解离通道分支比．在实验过程中，一束可调谐激光激发超声射流冷却的CS2分子到^1B2(^1∑u^+)电子态，光解产物CS用另一束可调谐激光通过激光诱导荧光(LIF)方法检测．通过拟合光解碎片激发谱的谱峰轮廓，获得了源于不同跃迁初始态的^1B2(^1∑u^+)态g振动能级的预解离寿命．通过分析CS的LIF光谱，则获得了不同光解波长下CS碎片的v=0—8振动态布居、v=1、4—8振动态的转动布居、能量分配以及两个预解离通道CS(X^1∑^+)+S(^3PJ)和CS(X^1∑^+)+S(^1D2)的分支比．实验还考察了初始态弯曲振动量子数v2″、振动角动量量子数l对解离动力学的影响．发现v2″的影响不大，而l的影响却是明显的．较大的l(=K)对应于较短的寿命和较小的通道分支比S(^3PJ)／S(^1D2)，即大的l(=K)有利于预解离的发生，同时更有利于产生S(^1D2)．     

空间光学的发展与波前传感技术

摘要：进入21世纪，国际上一些发达国家和有关部门都已制定了空间发展战略规划，如美国航空航天局（NASA）、欧洲空间局（ESA）和俄罗斯政府相关部门等都提出空间发展战略规划，这些规划提出了今后一段时间内空间科学要解决的问题和发展的方向，而解决这些问题并推进空间技术的发展很大程度上依赖于先进的光学和无线电望远镜及仪器设备。因此，本文介绍本世纪初国际上空间科学应用的大型天文望远镜的发展情况，重点描述了大口径光学望远镜的光学系统以及实现这类天文望远镜的关键技术之一一波前传感技术。     

Statefinder Diagnostic for Born--Infeld Type Dark Energy Model

Using a new method cafled the statefinder diagnostics which can make one dark energy model differ from the others, we investigate the dynamics of Born-Infeld （B-I） type dark energy model. The evolution trajectory of B-I type dark energy with Mexican hat potential model with respect to e-folding time N is shown in the r（s） diagram. When the parameter of noncanonical kinetic energy term η→0 or kinetic energy φ^2 →0, the B-I type dark energy （K-essence） model reduces to the quintessence model or the ACDM model corresponding to the statefinder pair （r, s） = {1, 0} respectively. As a result, the evolution trajectory of our model in the r（s） diagram in Mexican hat potential is quite different from those of other dark energy models. The current values of parameters Ωφ and wφ in this model meet the latest observations WMAP5 well.     

Observation Constraints on the Simplified GCG Model

A simplified version of generalized Chaplygin gas （GCG） as a dark energy model is studied. By using the latest 162 ESSENCE type Ia supernovae （She Ia） data, 30 high redshift She Ia data, the baryonic acoustic oscillation peak from SDSS and the CMB data from WMAP3, a strong constraint on this simplified GCG model is obtained. At the 95.4% confidence level we obtain 0.21 ≤ Ωm ≤ 0.31 and 0.994 〈 α 〈 1.0 with the best fit Ωm = 0.25 and a = 1. This best fit scenario corresponds to an accelerating universe with qo ≈-0.65 and z ≈ 0.81 （a redshiR of cosmic phase transition from deceleration to acceleration）.     

Constraints on Deceleration Parameter of a 5D Bounce Cosmological Model from Recent Cosmic Observations

We study the constraint on deceleration parameter q from the recent SNela Gold dataset and observational Hubble data by using a model-independent deceleration parameter q（z） = 1/2 - a/（1 ＋ z）^b under the flve-dimensional bounce cosmological model. For the cases of SNeIa Gold dataset, Hubble data, and their combination, the present results show that the constraints on transition redshift ZT are 0.35-0.07^＋0.14,0.68-0.58^＋1.47,and 0.55-0.09^＋0.18 with 1σ errors,respectively.     

Cylindrically symmetric inhomogeneous cosmological models with viscous fluid and varying Λ

Cylindrically symmetric non-static cosmological models representing a bulk viscous fluid distribution have been obtained which are inhomogeneous and anisotropic. Without assuming anyadhoc law, we obtain a cosmological constant as a decreasing function of time. Various physical and geometrical features of the models are also discussed.     

A Two-Field Dilaton Model of Dark Energy

We investigate the cosmological evolution of a two-field model of dark energy, where one is a dilaton field with canonical kinetic energy and the other is a phantom field with a negative kinetic energy term. Phase-plane analysis shows that the ＂phantom＂-dominated scaling solution is the stable late-time attractor of this type of model. We find that during the evolution of the universe, the equation of state w changes from w 〉 -1 to w 〈 -1, which is consistent with recent observations.     

Phantom Energy with Variable G and Λ

We investigate a cosmological model of a phantom energy with a variable cosmological constant （∧） depending on the energy density （ρ） as ∧∝ρ^α,α=const and a variable gravitational constant G. The model requires α 〈 0 and a negative gravitational constant. The cosmological constant evolves with time as ∧ ∝ t^-2. For ω 〉 - 1 and α 〈 -1 the cosmological constant ∧ 〈 0, G 〉 0 and ρ decrease with cosmic expansion. For ordinary energy （or dark energy）, i.e.ω 〉 -1, we have -1 〈 α〈 0 and β 〉 0 so that G〉0 increases with time and p decreases with time. Cosmic acceleration with dust particles is granted, provided -2/3 〈α〈 0 and ∧〉0.     

Observational Constraints on the Unified Dark-Energy--Dark-Matter Model

We investigate the constraints on a generalized Chaplygin gas （GCG） model using the gold sample type-Ia supernovae （She Ia） data, the new Supernova Legacy Survey （SNLS） Sne Ia data and the size of baryonic acoustic oscillation peak found in Sloan Digital Sky Survey （SDSS）. In a spatially flat universe case we obtain, at a 95.4% confidence level, A8 = 0.76^＋0.07 -0.07 and α= 0.028^＋0.322 -0.2382 Our results are consistent with the ACDM model （α= 0）, but rule out the standard Chaplygin gas model （α= 1）.     

Top ten accelerating cosmological models

Recent astronomical observations indicate that the Universe is presently almost flat and undergoing a period of accelerated expansion. Basing on Einstein's general relativity all these observations can be explained by the hypothesis of a dark energy component in addition to cold dark matter (CDM). Because the nature of this dark energy is unknown, it was proposed some alternative scenario to explain the current accelerating Universe. The key point of this scenario is to modify the standard FRW equation instead of mysterious dark energy component. The standard approach to constrain model parameters, based on the likelihood method, gives a best-fit model and confidence ranges for those parameters. We always arbitrary choose the set of parameters which define a model which we compare with observational data. Because in the generic case, the introducing of new parameters improves a fit to the data set, there appears the problem of elimination of model parameters which can play an insufficient role. The Bayesian information criteria of model selection (BIC) is dedicated to promotion a set of parameters which should be incorporated to the model. We divide class of all accelerating cosmological models into two groups according to the two types of explanation acceleration of the Universe. Then the Bayesian framework of model selection is used to determine the set of parameters which gives preferred fit to the SNIa data. We find a few of flat cosmological models which can be recommend by the Bayes factor. We show that models with dark energy as a new fluid are favoured over models featuring a modified FRW equation.