含有不同添加剂的明胶膜对Am（Ⅲ）／Eu（Ⅲ）的吸附研究

研究了分别添加γ-聚谷氨酸(γ-PGA)及1,4,7,10-四杂环十二烷基四乙酸(DOTA)的两种明胶膜对Am(Ⅲ)/Eu(Ⅲ)的吸附行为。结果表明,添加γ-PGA的明胶膜,在2.0 mol/L硝酸介质中,γ-PGA∶明胶的质量比为1∶5、吸附时间在15h以上时,对Eu3 的吸附率达38.6%,而对Am3 基本不吸附;添加DOTA的明胶膜,在2.0 mol/L硝酸介质中,DOTA∶明胶的质量比为1∶5、吸附时间在15h以上时,对Am3 的吸附率达41.3%,而对Eu3 的吸附率为5.1%。     

基于侧边抛磨光纤的表面布拉格光栅温度传感器

为了实现在侧边抛磨光纤（SPF）上制作布拉格光栅结构并提高器件设计灵活性,利用重铬酸盐明胶（DCG）作为光刻材料,提出一种新型的光纤表面布拉格光栅制作方法并对该器件温度传感特性进行研究。使用轮式抛磨系统制作SPF,并在SPF侧抛面上旋涂DCG,通过干涉光束曝光显影制作表面布拉格光栅。光谱测量表明:带有布拉格光栅的侧边抛磨光纤在1 480.2 nm处有透射谷,在相应位置反射谱有明显反射峰,其调制幅度达到15.9 dB,这是由于表面光栅的布拉格反射所致。温度传感实验表明,该布拉格反射峰的温度灵敏度为17.84 pm/℃。这种器件已在光纤传感和光纤滤波器等方面获得应用。     

免疫系统蛋白质相互作用的研究方法

对于相互作用蛋白的研究,有助于了解蛋白在细胞内如何发挥其生理功能.在人类基因组计划草图公布以后,基于蛋白质组学的蛋白谱研究逐渐得到重视,在此背景下,蛋白质相互作用的研究也逐步受到关注.对于蛋白质组学研究范围内所有蛋白质的相互作用的研究,被称作"相互作用组"[1].     

Non-parametric reconstruction of dark energy and cosmic expansion from the Pantheon compilation of type Ia supernovae

The equation of state(EoS) of dark energy plays an important role in the evolution of the universe and has attracted considerable interest in the recent years. With the progress in observational technique, a precise constraint on the EoS of dark energy can be obtained. In this study, we reconstruct the EoS of dark energy and cosmic expansion using Gaussian processes(GP) from the most up-to-date Pantheon compilation of type Ia supernovae(SNe Ia),which consists of 1048 finely calibrated SNe Ia. The reconstructed EoS of dark energy has a large uncertainty owing to its dependence on the second-order derivative of the construction. Adding the direct measurements of Hubble parameters H(z) as an additional constraint on the first-order derivative can partially reduce the uncertainty; however, it is still not sufficiently precise to distinguish between the evolving and the constant dark energy. Moreover, the results heavily rely on the prior of the Hubble constant H0. The H0 value inferred from SNe+ H(z) without prior is H0= 70.5 ± 0.5 km s~(-1) Mpc~(-1). Moreover, the matter density ?M has a non-negligible effect on the reconstruction of dark energy. Therefore, more accurate determinations on H_0 and ?_M are required to tightly constrain the EoS of dark energy.     

微系统热阻模型研究及其应用

系统级封装(SIP)实现了高密度、高集成度封装技术,同时散热问题备受关注,热设计中芯片结温预测十分重要.本文采用有限元仿真方法,建立了一种自然对流环境下微系统热阻模型,并通过模型中热阻矩阵预测多芯片总功耗相同条件下的各芯片结温,同时利用热阻测试试验和有限元仿真方法对预测结温进行验证,结果表明热阻矩阵模型预测芯片结温与热阻测试试验和有限元仿真结果误差分别小于2%和5%.但同时发现该热阻矩阵模型的不通用性,对于总功耗变化的多芯片结温,预测结果偏差较大.通过不同总功耗下各热阻矩阵的函数关系建立拟合曲线并修正热阻矩阵模型,修正后的结环境热阻矩阵适用于不同总功率条件、各芯片不同功率条件下的芯片结温预测,预测结果与热阻测试试验中芯片结温和有限元仿真结果误差均小于5%.因此,提出的修正结环境热阻矩阵的方法可以快速且便捷地预测不同功率芯片的结温,并对器件的散热性能进行较为准确的预估.     

Holographic Dark Energy Model is Consistent with Pantheon SN Ia Data

We constrain three cosmological models,i.e.,ACDM model, holographic dark energy(HDE) model and R_h = ct model by using the recent Pantheon compilation of type la supernovae(SN la), the direction measurements of Hubble parameter H(z), and the baryon acoustic oscillations(BAO). The spatial curvature is considered in the ACDM model and the HDE model. We show that the HDE model in a spatially flat and HDE dominate universe has the same behavior as Rh = ct model if the characteristic parameter of the HDE model C_0 approaches to infinity. Numerical results show that the ACDM model is the best favoured one among the three models. The HDE model is consistent with observational data, the best fitting value of C_0 is around 0.8, which implies that the Rh = ct model should be modified to be compatible with the present cosmological observational data. Combing all the datasets, we give strict constraint on the Hubble constant,where h_0=0.694 ± 0.020 for the ACDM model and h_0= 0.689 ±0.019 for the HDE model.Our results imply that the tension of Hubble constant between Planck collaborations and Riess et al. has been partially relaxed. The constraint on the spatial curvature is also given,where Ω_(k0) =-0.066 ± 0.165 for the ACDM model andΩ_(k0)=0.029 ± 0.067 for the HDE model.     

Testing the variation of the fine structure constant with strongly lensed gravitational waves

The possible variation of the electromagnetic fine structure constant, αe, at cosmological scales has aroused great interest in recent years. Strongly lensed gravitational waves(GWs) and their electromagnetic counterparts could be used to test this variation. Under the assumption that the speed of a photon can be modified,whereas the speed of a GW is the same as predicted by general relativity, and they both propagate in a flat FriedmanRobertson-Walker universe, we investigated the difference in time delays of the images and derived the upper bound of the variation of αe. For a typical lensing system in the standard cosmological models, we obtained B cosθ 1.85×10~(-5),where B is the dipolar amplitude and θ is the angle between observation and the preferred direction. Our result is consistent with the most up-to-date observations on αe. In addition, the observations of strongly lensed GWs and their electromagnetic counterparts could be used to test which types of alternative theories of gravity can account for the variation of α_e.     

一维光子晶体非线性微腔的缺陷模和双稳态

为了了解一维光子晶体布喇格非线性微腔产生的缺陷模和双稳态特性,采用数值模拟和理论分析相结合的方法,研究了缺陷层厚度变化和布喇格镜准周期性对缺陷模和双稳态的影响。研究结果表明,缺陷层厚度增大和折射率递增时,均可使缺陷模向低频方向移动,即布喇格腔共振模红移,因此,只要较小的入射光强就可使腔共振模红移到入射光模而产生阈值较低的双稳态,数值计算与理论分析是一致的。这对光子晶体微腔的设计有一定的意义。