大质量年轻星体新的C18O(1-0)发射

利用紫金山天文台青海观测站13.7米的毫米波望远镜对74个大质量年轻星体或候选进行了C^18O(1-0)的谱线观测。在63个源中观测到了C^18O(1-0)发射，其中57个天体第一次探测到C^18O(1-0)谱线发射。根据谱线辐射温度（TR^*)和半宽（△V），利用LTE方法计算了每个测量源的C^18O(1-0)发射的光学厚度和C^18O(1-0)分子的柱密度。讨论了^13CO(1-0)和C^18O(1-0)的谱线强度比和积分强度比。     

Advances in radiative transfer

This review describes advances in radiative transfer theory since about 1985. We stress fundamental aspects and emphasize modern methods for the numerical solution of the transfer equation for spatially multidimensional problems, for both unpolarized and polarized radiation. We restrict the discussion to two-level atoms with noninverted populations for given temperature, density and velocity fields. Unfortunately this article was originally published with typesetter's errors: The correct publication date was 25 February 2006, not 3 January 2006. The content was not in the final form. The publishers wish to apologize for this mistake. The online version of the original version can be found at /10.1007/s00159-005-0025-8.     

Geoeffective Analysis of CMEs Under Current Sheet Magnetic Coordinates

Using 100 CME–ICME events during 1997.01–2002.11, based on the eruptive source locations of CMEs and solar magnetic field observations at the photosphere, a current sheet magnetic coordinate (CMC) system is established in order to statistically study the characteristics of the CME–ICME events and the corresponding geomagnetic storm intensity. The transit times of CMEs from the Sun to the Earth are also investigated, by taking into account of the angle between the CME eruption normal (defined as the vector from the Sun center to the CME eruption source) and the Sun-Earth line. Our preliminary conclusions are: 1. The distribution of the CME sources in our CMC system is obviously different from that in the ordinary heliographic coordinate system. The sources of CMEs are mainly centralized near the heliospheric current sheet (HCS), and the number of events decreases with the increment of the angular distance from the CME source to the HCS on the solar surface; 2. A large portion of the total events belong to the same–side events (referring to the CME source located on the same side of the HCS as the Earth), while only a small portion belong to the opposite–side events (the CME source located on the opposite side of the HCS as the Earth). 3. The intense geomagnetic storms are usually induced by the same–side events, while the opposite side events are commonly associated with relatively weak geomagnetic storms; 4. The angle between the CME normal and the Sun–Earth line is used to estimate the transit time of the CME in order to reflect the influence of propagation characteristic of the CME along the Sun–Earth direction. With our new prediction method in context of the CMC coordinate, the averaged absolute error for these 100 events is 10.33 hours and the resulting relative error is not larger than 30% for 91% of all the events.     

On the possibility of investigation of the magnetic field structure in subphotospheric layers of the Sun according to observations of sunspot torsional oscillations

A method of investigation of the magnetic field structure in subphotospheric layers of the Sun has been developed. The method is based on observations of the torisonal oscillations of single sunspots. Characteristics of the torsional oscillations have been obtained from observations of the longitudinal magnetic field and radial velocities of seven single sunspots in the photospheric line Fe I λ5253 Å. The parameters of the torsional oscillations and magnetic tubes in the deep layers have been determined. The radius of the cross section of a magnetic flux tube forming a sunspot is greatest near the Sun’s surface and is approximately equal to the radius of a sunspot umbra. Down to the deeper layers, it decreases quite quickly. The longitudinal electric current appearing in the magnetic tube changes direction. The typical time of the current changes is determined by the period of the torsional oscillations. The intensity of the longitudinal magnetic field in the tube increases with depth. The Alfven wave velocity averaged over the length of a magnetic tube is tens or hundreds of times less than this velocity in a sunspot umbra. It decreases with an increase in the period of oscillations. A decrease in the Alfven wave velocity leads to an increase in the twisting angle of magnetic field lines.     

黄海冷水团海域微型异养鞭毛虫对异养细菌和蓝细菌摄食作用的初步研究

2006年10月在黄海冷水团海域的三个站点开展了微型异养鞭毛虫、异养细菌和蓝细菌的密度和生物量调查,进行了微型异养鞭毛虫的现场摄食实验,通过荧光标记细菌法和消化系数法获得该海区微型异养鞭毛虫对异养细菌和蓝细菌的摄食率,并估算了微型异养鞭毛虫对异养细菌和蓝细菌现存量及生产力的摄食压。结果显示,微型异养鞭毛虫、异养细菌和蓝细菌的密度分别为0.36×103~1.13×103,0.39×106~1.13×106和0.04×104~3.74×104cells/cm3,温跃层以上明显高于底层。微型异养鞭毛虫对异养细菌的摄食率为5.33~14.89个/(HF·h),对蓝细菌的摄食率为0.26×102~23.10×10-2cells/(HF·h),摄食率随深度而下降。微型异养鞭毛虫每天能消耗9.27%~33.08%的异养细菌现存量和8.12%~16.09%的蓝细菌现存量。同时,微型异养鞭毛虫对异养细菌和蓝细菌的日摄食量各占它们生产力的2.66%~13.10%和8.12%~16.09%。研究表明微型异养鞭毛虫的摄食可能不是秋季黄海冷水团海域浮游细菌及其生产力的主归宿。     

爆炸应力波作用下缺陷介质裂纹扩展的动态分析

采用透射式焦散线测试系统,进行爆炸应力波作用下缺陷介质裂纹扩展试验,研究了含与炮孔共线的预制裂隙介质裂纹扩展速度、加速度、裂纹尖端动态应力强度因子和动态能量释放率的变化规律以及它们之间的变化关系。试验结果表明,在爆炸应力波作用下裂隙两端产生了两条翼裂纹A、B,翼裂纹A的长度较翼裂纹B长,两条翼裂纹向相反的方向扩展;在翼裂纹扩展过程中,存在着加速与减速的过程,扩展速度瞬间达到峰值,其后逐渐振荡下降;动态应力强度因子也呈现瞬间达最大值到逐渐减小连续振荡变化的趋势,动态应力强度因子 > ;翼裂纹尖端的动态能量释放率对裂纹扩展具有驱动作用。     

综合物探在博格达山前古牧地复杂构造中的应用

准噶尔盆地南缘古牧地地区具有丰富的油气勘探潜力,但由于中深层地震成像存在盲区,长期以来对古牧地构造特征认识不清,制约了油气勘探进程.笔者采用高精度重磁和电法CEMP综合物探技术对古牧地地区构造特征进行了研究,取得了有价值的新认识.研究成果表明,古牧地构造为博格达山前褶皱冲断带的前锋构造,受阶梯状断裂控制.古牧地构造纵向上具多层构造特征,其中浅层为紧闭型逆冲倒转背斜,中层为受阶状逆冲断层控制的屋脊状断块,深层为潜山披覆型冲断背斜.重力异常显示古牧地背斜西围斜可能是一完整的背斜构造,古牧地中深层构造和古牧地背斜西围斜评价为有利的油气勘探目标.     

振动频率对饱和黏性土动力特性的影响

在回顾加荷频率对土样动力特性影响的研究基础上,采用某土石坝心墙防渗黏性土饱和试样,通过动三轴试验,研究了振动频率f对土样动力特性的影响。动强度试验结果表明：当 0.1～4 Hz时,动强度随f的升高而增大,但f继续升高后,动强度却有下降趋势。当 0.1～1.0 Hz时,频率愈高动孔压比愈大;当 1.0～6.0 Hz时,总的趋势为频率愈高,动孔压比愈小。表明频率较高时,动孔隙水压力来不及上升和扩散。较高频率f持续作用下,试样有吸水现象并伴随动孔压的下降。动模量阻尼试验结果是：f愈低,试样动变形开展愈充分;f愈高,动模量和阻尼比愈大。     

GPS遥感大气可降水量在大连地区3次降水过程中的应用

利用大连市气象局地基GPS/MET观测网大气可降水量（PWV）数据,分析2011年大连瓦房店、庄河和长海地区降水天气过程PWV的变化特征及其与降水量和降水强度的关系,在此基础上通过分析物理量场和天气系统,探讨大尺度水汽输送、辐合与PWV变化的关系及GPS在暴雨天气中的应用。结果表明：PWV的增长方式受当地天气系统的支配和制约,对一次明显的降水过程,从开始至结束PWV的变化与降水量有明显的相关性。当有水汽由南向北输送时,PWV在降水开始前逐渐增长,当地面及高空有大范围的水汽辐合且高空比湿值大于10 g·kg^-1时,PWV显著增长（降水开始前4-5 h）,主要降水时段与PWV峰值相对应,同时PWV的增幅大小与降水强度有明显的关系。