矿物英文名称的含意解析

许多矿物中文名称与英文名称的含意不一致，为了正确理解矿物的英文名称，本文介绍了３１０个常见矿物和重要矿物的英文名称的含意。     

罗氏沼虾线粒体锰超氧化物歧化酶的克隆表达与功能研究

罗氏沼虾(Macrobrachium rosenbergii)是我国重要的经济虾类之一。近年来, 细菌性感染造成罗氏沼虾养殖业病害频发, 经济损失巨大。因此了解其免疫机制对于指导疾病防控至关重要。线粒体锰超氧化物歧化酶(mitochondrial manganese superoxide dismutase, mMnSOD)被认为是抵御氧化应激的第一道防线, 在先天性免疫中具有至关重要的作用。目前, 甲壳动物中mMnSOD的免疫功能尚不清楚。为此, 本研究克隆了罗氏沼虾mMnSOD基因(mMnSOD of M. rosenbergii, MrmMnSOD), 制备了多克隆抗体, 分析了嗜水气单胞菌(Aeromonas hydrophila)感染下, MrmMnSOD在不同组织中的表达模式。结果显示, 肝胰腺和肠组织中MrmMnSOD的基因表达水平分别在感染后3h和6h达到最大; 组织免疫荧光分析显示, 肝胰腺和肠组织中MrmMnSOD均在感染后12h达到最大荧光强度。以上结果表明, mMnSOD参与了罗氏沼虾对嗜水气单胞菌的免疫应激反应。进一步的蛋白抑菌实验表明, MrmMnSOD可显著抑制大肠杆菌(Escherichia coli)、嗜水气单胞菌、副溶血弧菌(Vibrio parahaemolyticus)、金黄色葡萄球菌(Staphylococcus aureus)和无乳链球菌(Streptococcus agalactiae)的生长, 推测该蛋白可能属于免疫相关分子, 可通过抑菌反应发挥免疫功能。当前的研究结果进一步丰富了甲壳动物先天性免疫基础理论, 也可为今后罗氏沼虾的病害防控和药物研发提供新的靶点参考。     

乌干达Albert湖凹陷陡坡带成藏模式

乌干达Albert湖凹陷是世界上最年轻的生烃凹陷,至今仍处于断陷伸展阶段,特殊的地质背景使其具有独特油气富集特征。为了预测Albert湖西部陡坡带的勘探潜力,利用地震、钻井等资料开展了凹陷构造特征研究,系统分析了陡坡带石油地质条件和成藏模式。研究表明,板式陡坡带油气侧向运移,成藏条件优越;台阶式陡坡带以垂向运移为主,侧向运移为辅,成藏条件一般。运移和保存是Albert湖陡坡带油气富集的主控因素,西部陡坡带一台阶是有利勘探区带,资源潜力较大。此研究对非洲陆内裂谷油气勘探具有重要的指导作用。     

Numerical simulation of nonlinear dispersive waves propagating over a submerged bar by IB–VOF model

It is a good test for a numerical model to simulate progressive waves propagating over a submerged bar with a relatively high ratio of slopes. In this paper, the combined IB–VOF model is used to predict nonlinear dispersive waves propagating over a submerged bar with both slopes of 1:2. The predicted free surface elevations are compared with the experimental data and numerical results presented by other researchers. The comparison shows that the IB–VOF model is able to provide satisfactory wave profiles in the shallow water with strong nonlinear effects and in the wave transmitted region with strong wave dispersion in particular. Moreover, the wave evolution behind the submerged bar is described in detail, including the spatial wave profile modulation, spectral analysis of the time-series waves, flow velocity and pressure fields, and kinetic energy distribution. The effect of fluid viscosity on the numerical simulations is also studied, and it is found that the effect on the wave evolution considered in this paper is not significant. Finally, the hydrodynamic force acting on the bar is calculated using the IB–VOF model.     

基于扰动观测器的非奇异模糊滑模无人船编队控制

针对含有模型参数不确定性、外界干扰与抖振现象的无人船编队问题,提出了一种基于扰动观测器的非奇异模糊终端滑模编队控制方法。首先,将领航者–跟随者与人工势场法相结合,获得无人船的编队构型并保证无碰撞现象;其次,基于Lyapunov能量函数设计出模糊控制规则,消除了控制器中的抖振问题;进而,提出了一种扰动观测器来补偿未知动态和外界干扰,增强了系统的鲁棒性和稳定性。通过理论分析和仿真结果验证了所提控制方法的有效性。基于所设计的编队控制方法,无人船最终可形成期望的编队构型。     

空间VLBI的研究现状

评述了过去近三十年中空间VLBI的发展．其内容包括空间VLBI的简短发展历史,空间VLBI与地面VLBI的不同、空间VLBI的目前状况和空间VLBI的未来展望。着重介绍了作为首次空间VLBI的VSOP的各个方面情况,并给出了VSOP的连续谱、谱线普查样本,供参考。     

Eruption of an Active-Region Filament Driven by an Emerging Bipole

1 INTRODUCTION Filaments are cool, dense material suspended in the hot, tenuous corona. It is widely accepted that the global magnetic field surrounding the filaments plays a key role in their formation, structure and stability (Tandberg-Hanssen1995). Fil…     

Seven-frequency VLBI Observations of the GHz-Peaked-Spectrum Source OQ 208

We present quasi-simultaneous VLBI images of the GHz-Peaked-Spectrum radio source OQ 208 obtained with the Very Long Baseline Array at 1.4,1.7,2.3,5.0,8.4,15.4GHz and the European VLBI Network at 6.7 GHz.The low frequency(1.4,1.7 and 2.3GHz)ob- servations reveal a weak and extended steep-spectrum component at about 30mas away at position angle-110°,which may be a remnant emission.The radio structure of OQ 208 con- sists of two mini-lobes at 5.0,6.7,8.4 and 15.4 GHz.Our spectral analysis further confirms that the southwest lobe undergoes free-free absorption and finds that the free-free absorption is stronger in the inner region.By fitting the 8.4 GHz images from 1994 to 2005,we obtain a separation speed of 0.031±0.006 mas yr~(-1)between the two mini-lobes.This indicates a jet proper motion of 0.105±0.020 c and a kinematic age of 219±42 yr for the radio source.     

Variability of Extended Bipolar Regions

Using NSO/Kitt Peak synoptic charts from 1975 to 2003, we group the main solar magnetic fields into two categories: one for active regions (ARs) and the other for extended bipolar regions (EBRs). Comparing them, we find that there exist three typical characteristics in the variability of EBRs: First, there exists a correlation between ARs and EBRs. The phase of EBR flux has a delay nearly two CRs. Second, we find that the EBR flux has two prominent periods at 1.79 years and 3.21 years. The 1.79-year period seems to only belong to large-scale magnetic features. Lastly, the North – South asymmetry of EBR flux is not very significant on a time scale of one solar cycle. However, during solar maxima, its dominance is found to shift from one hemisphere to the other.     

Scattered emission from a relativistic outflow and its application to gamma-ray bursts

We investigate a scenario of photon scattering by electrons within a relativistic outflow. The outflow is composed of discrete shells with different speeds. One shell emits radiation for a short duration. Some of this radiation is scattered by the shell(s) behind. We calculate in a simple two-shell model the observed scattered flux density as a function of the observed primary flux density, the normalized arrival time delay between the two emission components, the Lorentz factor ratio of the two shells and the scattering shell's optical depth. Thomson scattering in a cold shell and inverse Compton scattering in a hot shell are both considered. The results of our calculations are applied to the gamma-ray bursts and the afterglows. We find that the scattered flux from a cold slower shell is small and likely to be detected only for those bursts with very weak afterglows. A hot scattering shell could give rise to a scattered emission as bright as the X-ray shallow decay component detected in many bursts, on a condition that the isotropically equivalent total energy carried by the hot electrons is large, ∼10⁵²–10⁵⁶ erg. The scattered emission from a faster shell could appear as a late short γ-ray/MeV flash or become part of the prompt emission depending on the delay of the ejection of the shell.