Discrepancy between infrared and optical emission in some Be stars

An expanding ring model is put forward to investigate the original regions of Hα line emission and infrared excess emission in Be stars, by taking optical depth into account. We find that the two regions depend strongly on the physical properties of the envelope of Be stars such as the initial density and density structure. This model can be used to qualitatively interpret the disagreement between the near infrared excess and the equivalent width (EW) of Hα emissionline, as observed in some Be stars.     

10Be/7Be implies the contribution of stratosphere-troposphere transport to the winter-spring surface O3 variation observed on the Tibetan Plateau

10Be/7Be is a stratospheric sensitive tracer.In this paper,measurements of 10Be/7Be and surface O3 from October 2005 to May 2006 at Mt.Waliguan (hereafter WLG,100.898°E,39.287°N,3810 m,a.s.l.),China global atmospheric watch (GAW) observatory,are introduced and used to investigate the stratosphere-troposphere transport (STT) and its impact on surface O3 on the Tibetan Plateau.The results show that the magnitude of STT is weak in winter,followed by strengthening from the end of winter to the middle of spring (from mid February to mid April) with large increases in 10Be,7Be,10Be/7Be and surface O3.At the end of spring (from the end of April to mid May in this paper),the STT weakened,and the continuous increase of surface O3 at WLG is produced by tropospheric photochemistry reactions.     

静电陀螺仪长球形空心转子径向变形设计

根据弹性力学薄壳理论的载荷弹性变形计算公式,应用小变形独立作用与合成原理,构建了静电陀螺仪空心转子表面径向载荷径向变形与离心载荷径向变形迭加的计算公式,并按径向变形迭加计算公式构造了两极长、赤道短的长球形空心转子。按径向变形设计的长球形空心转子,在高速旋转工作时能具有较为理想的圆球形。还以设计示例进行了说明。     

R矩阵法计算低能电子与Be+的碰撞激发

用二态密耦Ｒ矩阵方法,在入射电子能量约１－２０ｅＶ内,我们计算了电子与Ｂｒ＾＋碰撞的２ｓ→２ｓ,２ｐ弹性和激发截面,中列出了计算的结果,对比电子与Ｌｉ原子碰撞截面,详细讨论了各分波对截面的贡献。     

^7Be and ^210pb radioactivity and implications on sources of surface ozone at Mt. Waliguan

Beryllium-7 (^7Be) and lead-210 (^210Pb) radioactivity in aerosols collected, from October 2002 to January 2004 at Mt. Waliguan, by the Global Atmospheric Watch (GAW) Station, Qinghai Province is presented. The data were analyzed together with simultaneously measured surface ozone concentrations. We found that short time variations of ^7Be and ^210Pb were linked to alternations of synoptic weather around the Mt. Waliguan region. ^210Pb showed the lowest concentration in summer while ^7Be showed no obvious seasonal changes. Relatively high ^7Be and ^210Pb radioactivity was observed at Mt. Waliguan when compared with the observations at other mountain sites in other parts of the world. Surface ozone and ^7Be showed a consistent seasonal variation. Surface ozone correlated fairly well with ^7Be/^210Pb ratio. This suggested that vertical transport from higher altitudes of the atmosphere has predominant effects on the budget of surface ozone at Mt. Waliguan.     

古代书院的“明人伦”对现代高等院校德育教育的影响

古代书院在文化知识的传授与交流同时,贯穿于其中的是以“明人伦”为最终目标的书院教育理念。明人伦是指教会学生如何做人、追求完美道德、明白做人的道理,它曾对中国封建社会的教育产生过深刻的影响。现代社会“明人伦”较之传统社会“明人伦”的范围要大得多,研究这种教育理念对高等院校德育教育的影响并进行批判性地继承,从而探究其对现代...     

AgCu28对Be/HR-1不锈钢热静压接头组织性能的影响

以AgCu28合金作为中间层材料,进行Be/HR—I不锈钢热静压扩散连接。利用光学金相、扫描电镜(SEM)、俄歇电子能谱(AES)和X射线衍射仪(XRD)及材料试验机分析了热静压扩散连接接头的显微组织、元素和物相分布以及力学性能,探讨了扩散区成分、组织结构与性能的关系,以及AgCu28合金作为中间层材料的作用。研究表明:采用AgCu28合金作为中间层材料,能够实现Be/HR—I不锈钢的扩散连接,能有效地减少铍、不锈钢间的元素互扩散,减少了Be与Fe和不锈钢中其他合金元素的脆性金属间化合物的大量生成,接头质量较好。     

Growth ages of ferromanganese crusts from the western and central Pacific： Comparison between nannofossil analysis and ^10Be dating

Based on results of nannofossil analysis and 10Be dating in ferromanganese crusts M1-1 and A1-1 (no nannofossils were found in it),from the western and central Pacific respectively,it is found that the crust growth ages from nannofossil biostrati-graphy agree well with those based on 10Be isotope analysis. Both crusts have three growth layers,and the oldest layer was deposited in Miocene at about 12.80 Ma. The maximum,minimum,and average growth rates of crust A1-1 (from the central Pacific) are 8.11,1.92 and 3.47 mm/Ma,and those of crust M1-1 (from the western Pacific) are 2.93,0.47,and 0.94 mm/Ma.     

静电陀螺仪空心铍转子分析的一种等效载荷法

给出了一种等效载荷法,运用有限元分析软件对空心铍转子进行分析,得出在0.3~0.4 MPa下加工的转子工作时圆度较好,从而为加工长球形空心铍转子提供依据。     

基于EOPCB的芯片网络

就电光印制电路板(EOPCB)上的芯间光互连提出了一种网络化的连接方案.本方案力图减少芯片间连接线数,消除芯片的控制线及时钟线,通过介质访问技术实现芯片间的互连.该方案假设每个芯片只有一个光收发器(VCSEL/PIN),芯片网络由电气层供电,并通过光互连通信.在假设条件下,芯片网络可采用总线型、环型或星型物理拓扑结构连接.给出了上述拓扑结构网络连接光路实现方法,分析了光路损耗对芯片接入数目的限制,并就适于网络化光互连的光电集成电路(OEIC)芯片结构及介质访问方式作了简单讨论.     

Concentration and seasonal variation of 10Be in surface aerosols of Lhasa,Tibet

Thirty samples of total suspended particles were collected at a site in western part of Lhasa, Tibet from August 2006 to July 2007. The ¹⁰Be concentrations were determined by Accelerator Mass Spectrometer (AMS). Analysis of correlation between ¹⁰Be con-centrations and meteorological factors revealed that the wet scavenging has little effect on ¹⁰Be. ¹⁰Be can be used as a proxy of transport processes of the upper atmosphere over the Tibetan Plateau. Analysis of correlation between ¹⁰Be concentrations and NCEP reanalysis data demonstrated that higher ¹⁰Be concentrations in spring were probably caused by the atmosphere exchange from stratosphere to troposphere during February to June. Lower ¹⁰Be concentrations during August to September were consistent with the synchronous lower O₃ values, suggestive of both ¹⁰Be and O₃ were probably influenced by the atmosphere exchange from troposphere to stratosphere.     

Be_2二聚体分子形貌的理论研究

应用MP2、HF和B3LYP/6-311++G(3df,3pd),得到了Be2二聚体在单重态和三重态下的能量与核间距、电离能与核间距的关系曲线,并分析了这3种方法对其能量、电离能变化的影响;结合分子形貌理论详细介绍了单重态下,在核间距变化的过程中电子密度的变化趋势,形象地展示了由小的核间距到平衡位置再到较远的距离,即2个Be原子完全分开形成孤立原子的过程中,边界轮廓的大小和形状随着核间距变化的动态过程.这里使用MP2/6-311++G(3df,3pd)计算了第一电离能的变化趋势.使用MELD精密从头计算中的CISD/6-311++G(3df,3pd)方法,并结合我们自编的分子形貌程序,描绘出了Be2的分子内禀特征轮廓即分子形貌并计算了Be2的内禀特征参数,得到了很好的结果.     

7Be示踪内蒙古阴山北麓开垦草原土壤风蚀的尝试性研究

以放射性核素7Be为研究手段,对内蒙古阴山北麓开垦草原区春季土壤中的放射性核素7Be含量的连续性动态变化规律及土壤剖面中7Be含量的垂直变化特征进行了尝试性研究.由于7Be主要随降雨到达地表,而研究区春季(3~6月)降水很少,使得该时间段的7Be沉降量很小,在土壤表层没有形成明显的分布规律,因此,7Be不能作为估算开垦草原土壤风蚀量的示踪剂.     

静电陀螺仪空心球形铍转子的动态变形

利用有限元分析软件，对静电陀螺仪空心球形铍转子的4种典型结构进行离心变形的计算及变形仿真，讨论不同结构转子的动态变形及对圆球度误差的影响，提出了减小和补偿圆球度误差的措施。     

An X-ray outburst from the rapidly accreting young star that illuminates McNeil's nebula

Young, low-mass stars are luminous X-ray sources whose powerful X-ray flares may exert a profound influence over the process of planet formation. The origin of the X-ray emission is uncertain. Although many (or perhaps most) recently formed, low-mass stars emit X-rays as a consequence of solar-like coronal activity, it has also been suggested that X-ray emission may be a direct result of mass accretion onto the forming star. Here we report X-ray imaging spectroscopy observations which reveal a factor approximately 50 increase in the X-ray flux from a young star that is at present undergoing a spectacular optical/infrared outburst (this star illuminates McNeil's nebula). The outburst seems to be due to the sudden onset of a phase of rapid accretion. The coincidence of a surge in X-ray brightness with the optical/infrared eruption demonstrates that strongly enhanced high-energy emission from young stars can occur as a consequence of high accretion rates. We suggest that such accretion-enhanced X-ray emission from erupting young stars may be short-lived, because intense star-disk magnetospheric interactions are quenched rapidly by the subsequent flood of new material onto the star.     

基于参数微扰法精确计算铍离子Be2+和硼离子B3+的基态能量

建立含有屏蔽参数σ的铍离子Be~(2+)(z=4)和硼离子B~(3+)(z=5)的哈密顿方程.以有效核电荷数为z*=z-σ的类氢原子基态1s和激发态ns(n=2,3,…)组合的双电子波函数,作为铍离子Be~(2+)和硼离子B~(3+)的基态近似波函数.应用参数微扰法确定铍离子Be~(2+)的屏蔽参数σ=0.56350197和硼离子B~(3+)的屏蔽参数σ=0.525070444,应用参数微扰法计算铍离子Be~(2+)三级近似基态能量和硼离子B~(3+)四级近似基态能量的理论值与实验值的误差为ΔE≈10~(-4)~10~(-5)a.u..     

弹载星敏感器太空光环境研究

分析弹载星敏感器对星空成像时的太空光环境.运用普朗克黑体辐射定律,估算杂散光(太阳光、月亮光、地气光)在星敏感器工作高度处的辐照度;计算任意时刻星敏感器光轴与杂散光之间的夹角;综合考虑遮光罩的抑制杂散光作用,建立弹载星敏感器太空光环境的实时模型.仿真结果表明,星敏感器光轴与杂散光之间的夹角与实际情况吻合,该模型能够方便实时地估算弹载星敏感器的太空光环境,可为确定星敏感器的选星策略和导弹发射窗口提供依据.     

Vega is a rapidly rotating star

Vega, the second brightest star in the northern hemisphere, serves as a primary spectral type standard. Although its spectrum is dominated by broad hydrogen lines, the narrower lines of the heavy elements suggested slow to moderate rotation, giving confidence that the ground-based calibration of its visible spectrum could be safely extrapolated into the ultraviolet and near-infrared (through atmosphere models), where it also serves as the primary photometric calibrator. But there have been problems: the star is too bright compared to its peers and it has unusually shaped absorption line profiles, leading some to suggest that it is a distorted, rapidly rotating star seen pole-on. Here we report optical interferometric observations that show that Vega has the asymmetric brightness distribution of the bright, slightly offset polar axis of a star rotating at 93 per cent of its breakup speed. In addition to explaining the unusual brightness and line shape peculiarities, this result leads to the prediction of an excess of near-infrared emission compared to the visible, in agreement with observations. The large temperature differences predicted across its surface call into question composition determinations, adding uncertainty to Vega's age and opening the possibility that its debris disk could be substantially older than previously thought.     

三类恰当有效解集在正锥下的等价性和存在性

证明了Ge恰当有效解、Be恰当有效解和He恰当有效解在正锥下的等价性,且在此基础上,由在非空紧凸集上似凸多目标最优化问题的Ge恰当有效解的存在性,得出Be恰当有效解、He恰当有效解的存在性.     

Two populations of X-ray pulsars produced by two types of supernova

Two types of supernova are thought to produce the overwhelming majority of neutron stars in the Universe. The first type, iron-core-collapse supernovae, occurs when a high-mass star develops a degenerate iron core that exceeds the Chandrasekhar limit. The second type, electron-capture supernovae, is associated with the collapse of a lower-mass oxygen-neon-magnesium core as it loses pressure support owing to the sudden capture of electrons by neon and/or magnesium nuclei. It has hitherto been impossible to identify the two distinct families of neutron stars produced in these formation channels. Here we report that a large, well-known class of neutron-star-hosting X-ray pulsars is actually composed of two distinct subpopulations with different characteristic spin periods, orbital periods and orbital eccentricities. This class, the Be/X-ray binaries, contains neutron stars that accrete material from a more massive companion star. The two subpopulations are most probably associated with the two distinct types of neutron-star-forming supernova, with electron-capture supernovae preferentially producing systems with short spin periods, short orbital periods and low eccentricities. Intriguingly, the split between the two subpopulations is clearest in the distribution of the logarithm of spin period, a result that had not been predicted and which still remains to be explained.