三维地学模拟几个方面的研究现状与发展趋势

对三维地学模拟中的三维空间数据模型,三维地学模拟技术以及三维地学模拟软件的应用３个方面的研究现状进行了总结,并指出了发展趋势与研究思路。     

Optical observations of the Be/X‐ray transient system KS 1947+300

ROTSE‐IIId observations of the Be/X‐ray transient system KS 1947+300 obtained between September 2004 and December 2005 make it possible to study the correlation between optical and X‐ray activity. The optical outburst of 0.1 mag was accompanied by an increase of the X‐ray flux in the 2004 observations. A strong correlation between the optical and X‐ray light curves suggests that the neutron star directly accretes from the outflowing material of the Be star. The nearly zero time lag between X‐ray and optical light curves suggests a heating of the disk of Be star by X‐rays. No optical brightening and X‐ray enhancement was seen in the 2005 observations. There is no indication of an orbital modulation in the optical light curve. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

红外源IRAS 05437-0001和IRAS 05351+3549的CO分子谱线观测研究

利用紫金山天文台青海观测站13.7米射电望远镜对红外源IRAS05437-0001和IRAS05351+3549附近区域进行了CO(J=1-0)的分子谱线观测.发现在这两个源的方向都有很强的CO发射,CO谱线还有明显的线翼成分,这暗示两个红外源存在分子外流.同时还获得了每个源5＇×5＇的成图.通过对高速气体的空间分布的观测和分析,认为这两个源为分子外流源.其中IRAS05437-0001附近区域的外流结构比较复杂,可能这一区域的外流是多极的.IRAS05351+3549附近的外流结构较简单.从两个源的红外光谱分类以及外流的动力学时标得出都是年轻星(年龄～105yrs).通过对这两个外流源的参数估算,得出两个外流源的质量损失率.     

蛇绿岩及蛇绿岩构造侵位

已有研究实例阐明了蛇绿岩产出的构造环境及构造侵位机制的多样性 ,其中发育完整的蛇绿岩套具有与现代大洋岩石圈剖面相似的四层结构模式 ,它们形成于洋中脊扩张构造环境。由于构造运动使蛇绿岩套肢解 ,构造侵位于大陆造山带缝合线地带 ,沿断裂构造以构造岩片和构造混杂岩产出。蛇绿岩提供了洋壳形成和破坏的重要证据 ,蛇绿岩带或古缝合线是确定造山带中古洋盆存在及陆块边界的直接标志     

上海市地铁一号线隧道变形测量及规律分析

本文以上海市地铁一号线黄陂南路站近一年多种隧道变形测量采集整理分析为例,详细总结和讨论了地铁隧道变形测量的方法,对地铁一号线黄陂南路站附近上下行隧道变成进行了规律分析,同时对地铁一号线隧道运营以来整条隧道沉降变形规律进行了剖析。     

The spectral variations of the O-type runaway supergiant HD 188209

We report spectral time series of the late O-type runaway supergiant HD 188209. Radial velocity variations of photospheric absorption lines with a possible quasi-period of ∼6.4 d have been detected in high-resolution echelle spectra. Night-to-night variations in the position and strength of the central emission reversal of the H α profile occurring over ill-defined time-scales have been observed. The fundamental parameters of the star are derived using state-of-the-art plane-parallel and unified non-LTE model atmospheres, the latter including the mass-loss rate. The derived helium abundance is moderately enhanced with respect to solar, and the stellar masses are lower than those predicted by the evolutionary models. The binary nature of this star is not suggested either from Hipparcos photometry or from radial velocity curves.     

Magnetic confinement, magnetohydrodynamic waves and smooth line profiles in active galactic nuclei

In this paper, we show that if the broad-line region clouds are in approximate energy equipartition between the magnetic field and gravity, as hypothesized by Rees, there will be a significant effect on the shape and smoothness of broad emission-line profiles in active galactic nuclei. Linewidths of contributing clouds or flow elements are much wider than their thermal widths, because of the presence of non-dissipative magnetohydrodynamic waves and their collective contribution produce emission-line profiles broader and smoother than would be expected if a magnetic field were not present. As an illustration, a simple model of isotropically emitting clouds, normally distributed in velocity, is used to show that smoothness can be achieved for less than ∼8×10⁴ clouds and may even be as low as a few hundred. We conclude that magnetic confinement has far-reaching consequences for observing and modelling active galactic nuclei.     

Neon abundances in normal late-B and mercury–manganese stars

We make new non-local thermodynamic equilibrium calculations to deduce the abundances of neon from visible-region echelle spectra of selected Ne  i lines in seven normal stars and 20 HgMn stars. We find that the best strong blend-free Ne line that can be used at the lower end of the effective temperature T _eff range is λ 6402, although several other potentially useful Ne  i lines are found in the red region of the spectra of these stars. The mean neon abundance in the normal stars (log  A =8.10) is in excellent agreement with the standard abundance of neon (8.08). However, in HgMn stars neon is almost universally underabundant, ranging from marginal deficits of 0.1–0.3 dex to underabundances of an order of magnitude or more. In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is υ Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expected from radiative acceleration calculations, which show that Ne has a very small radiative acceleration in the photosphere, and that it is expected to undergo gravitational settling if the mixing processes are sufficiently weak and there is no strong stellar wind. According to theoretical predictions , the low Ne abundances place an important constraint on the intensity of such stellar winds, which must be less than 10⁻¹⁴ M_⊙ yr⁻¹ if they are non-turbulent.     

两种结构延绳钓渔具使用效果的比较研究--以金枪鱼(Thunnus)为例

分析比较两种不同结构的延绳钓渔具 1998年 2～ 9月期间在印度洋东部作业的生产效果。结果显示 ,钓具 A(平均放钓水深 90 .8m)与钓具 B(平均放钓水深 72 .7m)相比 ,钓捕效果差异显著 ,在渔获尾数、渔获重量、上钓率三个指标上 ,A钓具分别高于后者 2 9.52 %、30 .2 1%和9.80 %。提出了符合印度洋生产需要的钓具优化设计方案。     

Rotational contours of CH2X chain species compared with several diffuse interstellar bands

We have calculated synthetic spectra of perpendicular and parallel rovibronic bands of cumulene carbene molecules of the form C _n H₂. The perpendicular bands are consistent with a regularly spaced group of diffuse interstellar bands (DIBs) near 6850 Å. Parallel bands calculated for these molecular structures are consistent with the intrinsic profile of the associated 6614-Å DIB. Both types of bands are expected for an electronic transition that these species should have at those energies. We could not determine if the molecule was charged or if an atom other than carbon terminated the chain-end. Constraints due to molecular geometry and temperature place the chain length at 7–15 carbons to fit the 6850-Å group and 9–13 carbons to fit the 6614-Å DIB.