Screening and molecular classification of low-temperature protease from Antarctic microorganism and its characterization

107 strains producing protease were screened from 260 strains of Antarctic psychrophilic bacteria, among which proteolytic activity of five strains was more than 45 U ml^-1. The 16S rRNA gcne sequences homology and phylogcnetic analysis of five Antarctic psychrophillc bacteria showed that NJ276, NJS-9, NJ16-70,NJ345 belonged tO the described genus Pseudoalteromonas and NJ341 belonged to the genus Colwellia. The growth and the protease characteristic of four Antarctic psychrophilic bacteria had been studied, and the result showed that the 6ptimal temperature for growth and protease-produeing of four strains was about 10℃. Their growth and protease-produeing were still high during incubatlng 2-5 days. The maximum proteolytic activity occurred at pH 9 for four Antarctic psychrophilic bacteria. The optimal temperature of protease action of both strains NJ276 and NJ5-9 was about 50℃, however, the optimal temperature of protease aetlon of both strains NJ341 and NJ345 was about 40 ℃, and their proteolytic activity under 0℃ exhibited nearly 30% of the maximum activity, but their thermal stabilities were weaker. These results indicated that proteases from NJ341 and NJ345 were low-temperature proteases.     

光温敏雄性不育小麦的研究进展

何觉民等首先提出了改变小麦品种播种期、播种地获得雄性不育，用于生产杂交种的方法，并在贵农14中找到不育株，育成ES-3、ES-4、ES-5，从小偃、栽培二粒与普通小麦杂交后代中，获得一批不育株，育成一系列光温敏不育系。谭昌华等从栽培二粒小麦与普通小麦的杂交后代中，获得不育株，育成温光型雄性不育小麦CA9S,     

巨分子云聚合形成N体模拟中粒子数的效应

通过N体数值模拟以不同粒子数对星系中巨分子云的形成的影响进行了研究。结果表明：在聚合形成机制下，当对不同数目的分子云取相同的平均密度时，基本分子云的有效半径与其相应质量的立方根成正比，巨分子云的碎裂率与模拟基本分子云的数目无关。     

基于遗传克隆选择算法优化BP神经网络的地理信息预测研究

针对BP神经网络训练过程中的训练时间较长、完全不能训练或容易陷入局部极小值等问题,提出基于遗传克隆选择算法(CLOGA)优化BP神经网络的流程,克服BP算法的一些缺陷。并通过湖北省人口预测问题进行效果检验,得到满意的结果。     

水(冰):宇宙矿物

水(冰)是最简单的化合物,也是宇宙中丰度最大的矿物。通常认为,水无嗅、无味,无处不在。然而,液态水或固态水却是异乎寻常的物质。水具有某些其它物质没有的,特别是赋予生命所要求的特殊性质,如氢键、水簇和kosmotrope离子等。本文综述水(冰)的结构、化学性质、物理性质、分布以及与生命的关系。     

岩石本构模型智能辨识方法研究

岩石本构模型是研究岩石力学特征和变形机制的基础,而本构模型或模型中相关参数的识别是本构模型研究中的热点和难点问题。本文基于红板岩室内力学实验数据,分别利用遗传算法、BP神经网络以及遗传规划对红板岩本构模型进行了模式识别,结果表明,遗传算法进行参数识别需要事先假定流变模型的形式,误差较大,而BP神经网络和遗传规划可以一次性同时确定流变模型的结构形式及参数,有效避免模型假定所带来的误差。而遗传规划与BP神经网络相比,具有精度高、收敛快,可视化程度高等特点,为岩石本构参数及模型的智能识别方法的选取提供参考。     

对59个北天EGO天体方向上的分子云~(12)COJ=2-1和J=3-2频谱观测研究

为了研究有大质量恒星形成的分子云与其它分子云之间的差异,对北天的59个作为大质量恒星形成区的Spitzer延展绿色天体(Extended Green Objects,简称EGOs)视线方向进行了分子云~(12)CO J=2-1和J=3-2频谱观测,并与文献中对同一批天体方向观测得到的~(12)CO J=1-0频谱数据合并进行分析.对与EGO天体成协的分子云(简称EGO分子云)和其它non-EGO分子云进行了CO多跃迁谱线强度和宽度的统计比较分析.在数据统计的基础上,讨论了这两类分子云的气体温度分布、密度分布、速度场分布对观测数据统计特征的影响.分析结果表明,直接决定是否有大质量恒星形成的关键因素可能并不是巨分子云的质量是否足够大,而是巨分子云的引力塌缩程度足否充分(即分子云团块的体积填充因子是否足够大).     

IRAS 20231+3440区外流激发源的性质研究

给出红外点源IRAS 20231 3440附近恒星形成区近红外．JHK’和H2成像观测结果，以及与该IRAS点源成协的近红外点源IRS1的K波段分光观测结果．．JHK’观测显示该区域存在嵌埋的年轻星天体，H2窄波段观测揭示了若干个氢分子发射结点，其中有几个结点排列成线形，暗示分子氢喷流的存在．喷流的北部与已知观测的分子外流成协，表明二者之间存在联系．喷流的走向提示IRS1可能是其激发源，对IRS1的K波段分光观测给出了进一步的证据．从近红外、MSX及IRAS资料估计出IRS1的能谱分布，表明它是一个处于ClassI状态的中等质量的年轻星天体．     

Molecular Gas and Dust in the Massive Star Forming Region S 233 IR

The massive star forming region S 233 IR is observed in the molecular lines CO J = 2-1, 3-2, NH3 (1,1), (2,2) and the 870#m dust continuum. Four submillimeter continuum sources, labelled SMM 1-4, are revealed in the 870μm dust emission. The main core, SMM1, is found to be associated with a deeply embedded near infrared cluster in the northeast; while the weaker source SMM2 coincides with a more evolved cluster in the southwest. The best fit spectral energy distribution of SMM1 gives an emissivity of β = 1.6, and temperatures of 32 K and 92 K for the cold- and hot-dust components. An SMM1 core mass of 246 M⊙ and a total mass of 445 M⊙ are estimated from the 870μm dust continuum emission.SMM1 is found to have a temperature gradient decreasing from inside out, indicative of the presence of interior heating sources. The total outflow gas mass as traced by the CO J = 3-2 emission is estimated to be 35 M⊙. Low velocity outflows are also found in the NH3 (1,1) emission. The non-thermal dominant NH3 line width as well as the substantial core mass suggest that the SMM1 core is a “turbulent,massive dense core”, in the process of forming a group or a cluster of stars. The much higher star formation efficiency found in the southwest cluster supports the suggestion that this cluster is more evolved than the northeast one. Large near infrared photometric variations found in the source PCS-IR93, a previously found highly polarized nebulosity, indicate an underlying star showing the FU Orionis type of behavior.