Neutron irradiation and post-irradiation annealing of rutile (TiO2−x ): effect on hydrogen incorporation and optical absorption     

Geoffrey David Bromiley  Andrei A. Shiryaev 《Physics and Chemistry of Minerals》2006,33(6):426-434

Neutron irradiation and post-irradiation annealing under oxidising and reducing conditions have been used to investigate H incorporation in, and the optical properties of, reduced (TiO_2−x ) rutile. Optical absorption in rutile is mainly due to a Ti³⁺ Ti⁴⁺ intervalence charge transfer effect. The main mechanism for H incorporation in rutile involves interstitial H not coupled to other defects, which has important implications for the rate of H diffusion, and possibly also on the electrical properties of rutile. Additional minor OH absorption bands in IR spectra indicate that a small amount of interstitial H is coupled to defects such as Ti³⁺ on the main octahedral site, and indicates that more than one H incorporation mechanism may operate. Concentration of oxygen vacancies has a controlling influence on the H affinity of rutile.  相似文献   

Thermal expansion and crystal structure of FeSi between 4 and 1173 K determined by time-of-flight neutron powder diffraction     

L. Vočadlo  K. S. Knight  G. D. Price  I. G. Wood 《Physics and Chemistry of Minerals》2002,29(2):132-139

The thermal expansion and crystal structure of FeSi has been determined by neutron powder diffraction between 4 and 1173?K. No evidence was seen of any structural or magnetic transitions at low temperatures. The average volumetric thermal expansion coefficient above room temperature was found to be 4.85(5)?×?10^?5?K^?1. The cell volume was fitted over the complete temperature range using Grüneisen approximations to the zero pressure equation of state, with the internal energy calculated via a Debye model; a Grüneisen second-order approximation gave the following parameters: θ_D=445(11)?K, V ₀=89.596(8)?ų, K ₀′=4.4(4) and γ′=2.33(3), where θ_D is the Debye temperature, V ₀ is V at T=0?K, K ₀′ is the first derivative with respect to pressure of the incompressibility and γ′ is a Grüneisen parameter. The thermodynamic Grüneisen parameter, γ_th, has been calculated from experimental data in the range 4–400?K. The crystal structure was found to be almost invariant with temperature. The thermal vibrations of the Fe atoms are almost isotropic at all temperatures; those of the Si atoms become more anisotropic as the temperature increases.  相似文献   

新技术在北极星天文方位角测量中的应用     

赵珞成  熊瑛 《测绘信息与工程》2003,28(3):37-39

使用GPS接收机的UTC作为北极星天文方位角测量的时间比对的标准时间，利用推估UTl与UTC的差值，将时间归算到UTl的方法，可满足各等级天文方位角测量的要求，现场计算零点恒星时和北极星坐标的精度满足北极星天文方位角测量的要求，实现了现场评估测量精度。  相似文献   

An Unusual Texture: Skeletal Sphalerite in Pyrite from Dajing Tin-polymetallic Deposit, China     

Yu Wang Wang    Jing Bin Wang  Li Juan Wang 《Resource Geology》2003,53(1):67-72

Abstract. Skeletal sphalerite with stellar, cruciform and snowflake-like (or cauliflower-like) shapes included in pyrite is widely found in the Dajing tin-polymetallic deposit. It occurs only in chalcopyrite-pyrite mineralization stage. The compositions of all sphalerites in the chalcopyrite-pyrite stage are characterized by high Cu content (3.9 - 7.0 wt% with a mean of 5.4 wt%), while the skeletal crystal sphalerite has higher zinc and cadmium contents, and lower copper and iron contents, compared with other sphalerites of the same stage. The skeletal crystal sphalerite in pyrite is possibly generated by exsolution.  相似文献   

AEKF在星敏感器低频误差补偿中的应用   总被引：1，自引：0，他引：1  

雷琦  龚志辉  林雕  耿弘毅 《测绘科学技术学报》2016,(3):252-257

高分辨率对地观测卫星需要精确的姿态信息来满足后续对地定位等工作,因此姿态确定精度十分重要。星敏感器的低频误差是影响卫星姿态确定精度的重要因素之一,主要是由空间周期性的热环境变化引起的。为进一步提高卫星姿态确定精度,对星敏感器的低频误差产生机理即星敏感器主光轴做周期性扰动进行了分析,设计了星敏感器低频误差补偿方案,建立了考虑星敏感器低频误差在内的组合定姿模型,利用拓维卡尔曼滤波(AEKF)对低频误差进行补偿,并引入RTS平滑滤波进一步提高姿态确定精度。仿真实验表明,设计的星敏感器低频误差补偿方案能有效对其进行补偿,提高卫星姿态确定精度。  相似文献   

Halin图的色数问题     

朱建  陈丽娟 《南京气象学院学报》2016,8(3):286-288

Halin图G=T∪C,其中T为每一非悬挂点(内点)度数至少为3的平面树,C为连接T的所有悬挂点的圈.文章分别讨论了Halin图的星色数、面色数及分数色数.  相似文献   

建成环境对星级酒店内被盗的影响——以ZG市中心城区为例   总被引：1，自引：0，他引：1  

张春霞  周素红  柳林  肖露子 《地理科学进展》2020,39(5):829-840

盗窃是中西方酒店内财产犯罪中最为高发的一种,但鲜有研究关注建成环境对酒店被盗的影响。论文以2012—2014年ZG市中心城区发生过被盗的星级酒店作为研究样本,在综合分析酒店被盗时空特征的基础上,选取酒店周围500 m范围内的建成环境指标,利用负二项回归模型,对分时段各类型的星级酒店被盗的影响因素进行系统建模分析。结果表明：被盗星级酒店的时空分布呈现典型的集聚分布特征。不同时段空间“主热点”分布相对稳定,“次热点”有所不同。整体来看,提高服务水平对降低星级酒店被盗的作用最为稳定,周围的兴趣点(Point of Interest, POI)数量会显著增加星级酒店被盗的机会,道路交叉口则对星级酒店被盗起显著监管作用。分模型结果显示,服务水平对三星级和五星级酒店被盗的抑制作用显著,道路交叉口则对以商务客人为主的四星级酒店被盗的抑制作用更强,而POI数量对等级较低的三星、四星酒店被盗作用更为明显;大型零售商业中心能显著增加旅游旺季及周末时段的酒店被盗的数量,道路交叉口数量则对旅游淡季、工作日2个时段的星级酒店被盗风险的监控作用显著。研究表明建成环境在影响ZG市星级酒店被盗的机会和成本方面作用显著。结果验证了日常活动理论在中国大城市星级酒店被盗方面研究的适用性,拓展了犯罪地理学在星级酒店被盗方面的研究成果,对酒店盗窃预防有指导意义。  相似文献   

GRB 170817A的洛伦兹因子和观测角          下载免费PDF全文

林一清 《天文学报》2020,61(1):6

伴随着引力波事件GW170817的短暴GRB (Gamma-Ray Burst) 170817A首次提供了双中子星并合与短暴相联系的直接证据.但是短暴GRB 170817A具有非常弱的光度,意味着观测的视线方向可能偏离喷流轴方向.根据短暴静止系的峰值能量E_(p,i)和各向同性光度L_(iso)。之间的关系以及洛伦兹因子Γ和L_(iso)。之间的关系估算了短暴GRB 170817A以及长短暴GRB 060614观测角与喷流边缘的夹角θ'_(obs)和洛伦兹因子Γ,结果表明GRB 170817A的Γ=45±27,θ'_(obs)=2.2±0.5°,而GRB 060614的Γ=214±93,θ'_(obs)=0.5±0.1°.这个结果相当于GRB 170817A的正轴各向同性光度L_(iso,on)=(2.1±0.7)×10~(49) erg·s~(-1),比典型的短暴少2-3个数量级.GRB 060614的L_(iso,on)=(5.12±1.91)×10~(51) erg·s~(-1)与典型短暴相当.这意味着GRB 060614可能属于短暴类型,而GRB 170817A可能本质上就是一个弱暴.  相似文献   

基于DEM数据的巴丹吉林沙漠沙丘分布规律及其形态参数   总被引：2，自引：2，他引：0  

汪克奇  赵晖  王兴繁  杨宏宇  晁倩 《中国沙漠》2020,40(4):81-94

沙丘形态特征是风沙地貌研究的重要内容。数字高程模型（DEM）因卓越的三维地形表达能力被广泛应用于沙丘形态研究中。长期以来,受交通条件和研究方法的制约以及高大沙山分布位置的限定,对巴丹吉林沙漠沙丘形态的研究主要集中在沙漠东南部,缺乏对整个沙漠沙丘分布规律及其形态参数特征的系统认知。而对整个沙漠沙丘形态特征的研究,是区域风沙地貌形成与演化研究的重要组成部分。以巴丹吉林沙漠内所有独立沙丘为研究对象,利用研究区DEM数据和一种新的算法,研究了沙漠内两种主要类型沙丘（横向沙丘、星状沙丘）的分布规律及其形态参数特征。结果表明：沙漠内独立沙丘大约有6 033座,高度9~433 m,高度超过350 m的巨型沙山共有53座,其中星状沙山7座,最大高度383 m;横向沙山46座,最大高度433 m。横向沙丘高度与等效沙丘厚度呈正相关的线性函数关系,星状沙丘高度与等效沙丘厚度呈正相关的对数函数关系,表明在现代气候和环境条件下,横向沙丘高度仍在增加,而星状沙丘高度增长已经趋缓。两类沙丘的主轴向大都垂直于研究区主风向NW-SE。横向沙丘起沙风风向单一,沙丘轴向集中在NE-SW和NNE-SSW方向;星状沙丘起沙风风向略为复杂,沙丘存在多个次级轴向。  相似文献   

Molecular clouds and the formation of open clusters     

B. Stecklum 《Astronomische Nachrichten》1989,310(5):375-379

Using analytical approximations of the mass spectra of molecular clouds and stellar systems including open clusters and associations a relation between the final star formation efficiency (final SFE) and the initial cloud mass is derived. The dependence of the SFE on cloud mass is estimated for two cases of molecular cloud destruction by stellar winds in spherical geometry. The result of growing SFE with rising cloud mass does not agree with current observations and the above relation. A decrease of the SFE is expected if the fraction of high-mass stars grows with increasing mass of the cloud.  相似文献