Researches on the Internal Molecular Weight Uniformity of Chitosan Biomaterials

Uniform molecular weight(Mw)chitosan(CS)is highly demanded in medical biomaterial industry.This present article described heterogeneous degradation of CS in aqueous HCl/ethanol solution,in which progress uniform Mw CS was successfully prepared.The Mw distribution of CS was measured by gel permeation chromatography(GPC)analysis.Moreover,the structure and properties of degraded CS were characterized by Fourier transform infrared spectroscopy(FT-IR),nuclear magnetic resonance spectroscopy(^1H NMR),X-ray diffraction(XRD)and thermogravimetric(TG)analysis.In addition,the biocompatibility of degraded CS was also assessed by hemolysis rate(HR)measurement.The Mw of CS dramatically decreased from 246 KDa to 76 k Da at the initial 30 min,and stabilized at 18 kDa after 24 h.GPC analysis results showed that the degraded CS molecular become homogenization.FT-IR and 1 H NMR analysis confirmed the basic structure of CS molecular backbone was not destroyed during this progress.Besides,the water solubility of CS was not significantly influenced by this reaction.Moreover,the XRD analysis revealed that crystallinity of degraded CS increased from 70.32% to 99.25%with time.The TG analysis showed improved thermal stability of degraded CS.HR measurement demonstrated the degraded CS possessed excellent biocompatibility.This simple and efficient heterogeneous degradation would open up a new route to produce uniform Mw CS.     

济阳坳陷古近纪沟鞭藻分子化石的分布与控制因素

济阳坳陷古近纪沟鞭藻化石十分丰富,沟鞭藻为有机质富集层的形成作出了重要贡献。三芳甲藻甾烷和甲藻甾烷是沟鞭藻及其祖先在古代沉积物中两种重要的存在形式,并且它们几乎专一性地由沟鞭藻提供。研究发现,沟鞭藻的不同属种,德弗兰藻属、多刺甲藻属、渤海藻类等,均可以提供丰富的三芳甲藻甾烷和甲藻甾烷,但是三芳甲藻甾烷和甲藻甾烷对沉积环境的变化具有不同的响应。在淡水、半咸水、咸水等不同水介质条件下,三芳甲藻甾烷指数稳定分布在0.50～0.96之间,高丰度的三芳甲藻甾烷与地层中丰富的沟鞭藻化石相一致,因而三芳甲藻甾烷是指示沟鞭藻输入的有效分子化石。甲藻甾烷的丰度与古沉积环境存在密切关系,高盐环境有利于甲藻甾烷的形成和保存,随着盐度的降低甲藻甾烷指数在0.04～0.74这样一个较大的范围内变化,其发育程度与有机质沉降过程中和成岩作用早期遭受的微生物降解作用有关,强烈的生物降解不利于甲藻甾烷的保存。     

Cosmic-ray positrons: are there primary sources?

Galactic cosmic rays consist of primary and secondary particles. Primary cosmic rays are thought to be energized by first order Fermi acceleration processes at supernova shock fronts within our Galaxy. The cosmic rays that eventually reach the Earth from this source are mainly protons and atomic nuclei, but also include electrons. Secondary cosmic rays are created in collisions of primary particles with the diffuse interstellar gas. They are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy Antimatter Telescope (HEAT) balloon-borne instrument, we have measured the abundances of positrons and electrons at energies between 1 and 50 GeV. The data suggest that indeed a small additional antimatter component may be present that cannot be explained by a purely secondary production mechanism. Here we describe the signature of the effect and discuss its possible origin.     

Rovibrational excitation of HD in collisions with atomic and molecular hydrogen

We have computed cross-sections and rate coefficients for rovibrational transitions in HD, induced by collisions with atomic and molecular hydrogen. We employed fully quantum-mechanical methods and the potential of Boothroyd et al. for H–HD, and that of Schwenke for H₂–HD. The rate coefficients for vibrational relaxation v =1→0 of HD are compared with the corresponding values for H₂. The influence of vibrationally excited channels on the rate coefficients for rotational transitions within the v =0 vibrational ground state of HD is shown to be small at T =500 K, where T is the kinetic temperature. The rate coefficients, for 100 T 2000 K, are available from http://ccp7.dur.ac.uk/.     

13mm低温制冷谱线接收系统和星际水分子观测研究

为了开拓短厘米波单天线星际分子的观测和研究,在乌鲁木齐天文站２５ｍ射电望远镜１３ｍｍ低温制冷接收机的基础上,配置了声表面波频谱仪和谱线数据采集系统,组成了１３ｍｍ低温致冷谱线接收机．接收机前端是一个工作在低温２０Ｋ的低噪声放大器,本振是２２ＧＨｚ的锁相源．接收机的平均噪声温度为５０Ｋ．后端是一个宽带的（４０ＭＨｚ）高分辨率（４０ｋＨｚ）的声表波频谱仪．利用这套系统观测了一批已知的水脉泽源,观测系统正常,结果合理．观测结果表明,乌鲁木齐天文站良好的站址和２５ｍ射电望远镜给厘米波段星际分子谱线观测提供了一个很好的条件．     

新疆北部泥盆系遗迹化石共生组合关系及其古环境和古生态意义

作者通过对新疆北部泥盆纪火山－沉积岩系中６个习性类、９种遗迹群落中２８个遗迹属的野外和室内观测,首次从遗迹化石个体或群体间排列状态和空间分布角度提出了遗迹化石共生组合关系的概念,并将其区分为３类１５型．遗迹化石共生组合关系的研究对详细的古环境、古生态分析和对蕴含在遗迹化石中尚未揭示的奥秘的探索有重要意义．     

基于网络药理学和分子对接技术探究柯里拉京治疗卵巢癌的关键靶点及分子机制

目的：采用网络药理学和分子对接技术相结合的方法探究柯里拉京（Cor）治疗卵巢癌的关键作用靶点和分子机制。方法：利用PharmMapper、TargetNet及Swiss Target Prediction在线工具预测Cor的作用靶点,通过OMIM、TTD、CTD、DisGenet、PharmGKB及MalaCards数据库获取卵巢癌相关的疾病靶点,并将药物靶点与疾病靶点取交集得到Cor治疗卵巢癌的预测靶点。借助STRING数据库、Cytoscape 软件构建蛋白质-蛋白质相互作用（PPI）网络,并采用CentiScape插件筛选出PPI网络中的核心靶点。运用GEPIA和Kaplan-Meier Plotter在线平台分别对这些核心靶点进行基因表达差异分析和生存分析,以明确Cor治疗卵巢癌的关键靶点。利用DAVID数据库进行基因本体（GO）功能及京都基因与基因组百科全书（KEGG）通路富集分析。运用Autodock Vina软件进行正向分子对接,预测关键靶点和Cor之间的结合活性。结果：Cor治疗卵巢癌的预测作用靶点共24个,其中RAC-α丝氨酸/苏氨酸蛋白激酶(AKT1)、表皮生长因子受体(EGFR)、雌激素受体1(ESR1)、原癌基因酪氨酸蛋白激酶(SRC)是Cor治疗卵巢癌的关键靶点,主要涉及血管内皮生长因子(VEGF)信号通路、缺氧诱导因子-1(HIF-1)信号通路及叉头样转录因子(FoxO)信号通路,可能通过调控细胞凋亡、细胞增殖、血管内皮细胞迁移等生物过程而发挥治疗卵巢癌的作用。分子对接结果显示,Cor与预测靶点之间具有较好的亲和力,表明通过网络药理学预测作用靶点的方法具有良好的可靠性。结论：Cor是通过多靶点、多通路的协同作用来干预多个生物过程,从而发挥其抗卵巢癌疗效,为进一步研究其治疗卵巢癌的分子机制提供了新的线索。     

基于网络药理学和分子对接探析养心活血通脉汤治疗稳定性冠心病的作用机制

目的：运用网络药理学和分子对接技术探析养心活血通脉汤治疗稳定性冠心病的作用机制。方法：应用TCMSP、Herb、TCMID平台检索养心活血通脉汤成分及作用靶点;经GeneCards、OMIM、DisGeNET平台获取稳定性冠心病靶点;运用Cytoscape 3.9.1建立“药物-活性成分-靶点”网络及蛋白质-蛋白质相互作用（PPI）网络,筛选核心靶点。由Metascape平台进行基因本体（GO）功能和京都基因与基因组百科全书（KEGG）通路富集分析。利用Auto Dock Tools软件进行有效成分与和核心靶点分子对接。结果：养心活血通脉汤治疗稳定性冠心病主要成分为槲皮素、山柰酚、β-谷甾醇、芒柄花黄素、黄芩素、丹参酮ⅡA,关键靶点为肿瘤坏死因子（TNF）、白细胞介素-6（IL-6）、丝氨酸/苏氨酸激酶1（AKT1）、白细胞介素-1β（IL-1β）、血管内皮生长因子（VEGFA）,关键通路为脂质和动脉粥样硬化（Lipid and atherosclerosis）、磷脂酰肌醇3激酶-丝氨酸/苏氨酸蛋白激酶1信号通路（PI3K-Akt信号通路）、肿瘤坏死因子信号通路（TNF信号通路）、丝裂原活化蛋白激酶信号通路（MAPK信号通路）、糖基化终产物/受体信号通路（AGE-RAGE信号通路）等。分子对接结果显示各有效成分与各核心靶点结合活性较好。结论：养心活血通脉汤治疗稳定性冠心病作用机制主要为降脂、抗动脉粥样硬化、抗炎、抗心肌损伤。     

基于经验模式给定热层温度对热层大气密度反演影响的评估

利用加速度计数据反演热层大气密度算法一般需由经验模式给定热层大气温度,进而计算大气阻尼系数C_D.本文基于CHAMP卫星加速度计数据反演得到大气密度,以2008年为例,利用反演得到的热层大气密度循环迭代修正大气阻尼系数C_D,通过对比修正前后密度偏差,评估经验模式给定热层温度对热层大气密度反演造成的影响.结果表明,经验模式热层温度计算偏差对大气密度反演造成的影响小于5%,而且考虑大气成分的改变则进一步降低了这种影响.