一个陆面过程参数化模式与 MM5的耦合

在法国陆面过程模式的基础上,为了表示冠层叶片遮挡对水分蒸发阻抗的影响,在植被覆盖部分引入了遮盖因子,然后将这个修正的陆面过程参数化模式耦合到MM5模式中。耦合后的模式模拟出了因为降水造成土壤湿度变化和植被覆盖动态作用对地面通量的影响,而原MM5模式模拟结果则没有反映上述动态变化对地面通量的作用。原MM5模式和耦合模式模拟了1993年8月17日到20日以内蒙古半干旱草原为中心的中尺度区域的气象场,模拟结果和IMGRASS预观测资料进行了对比,对比说明新的陆面过程模式提高了MM5模式对地面通量和边界层各物理量（风、温、湿）的模拟精度。     

垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.——碱蓬属一新种

报道了中国碱蓬属植物一新种——垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.。该种与南方碱蓬Suaeda australis(R.Br.)Moq.相近,但系一年生,种子具圆盘状和卵形两种形状,直径约2～3mm,叶长可达5～7 cm,无不定根,与南方碱蓬相区别。垦利碱蓬生长于潮间带和海水周期性淹没处。耐高盐,区域内海水盐度为25,滩涂表层含盐量在退潮后经日晒蒸发可达60‰以上。常形成单一种群的红海滩植被景观。模式标本存:中国科学院海洋生物标本馆;编号:MBM286537。采集地:莱州湾垦利海域潮间带泥滩。采集人:邢军武、曲宁、钟芳。     

青岛地区海雾分布及大气边界层条件分析

青岛地区海雾多发,观测表明海雾对沿海地区影响范围不尽相同,特别是海雾影响内陆的机理尚缺乏研究。本文利用观测资料及数值模式统计了青岛地区4月-7月海雾分布特征,并对不同影响范围海雾典型个例进行对比分析,结果表明:海雾发生日数自沿海向内陆递减。胶州湾沿岸雾日数比黄海沿岸明显减少,胶州湾东北部的雾日数要少于胶州湾西北部。海雾多发生于高空形势稳定,低层偏南流场的天气条件下。大气边界层内逆温层的的范围大致影响着海雾的分布。只影响沿海的海雾,地面为偏南风,风速在3~8 m/s之间,内陆风力减弱不明显。500 m以下大气边界层内风速切变大。湍流作用使海雾向内陆推进过程中倾斜抬升为低云,地面雾区减弱。能够影响内陆地区的海雾,多出现在地面风力较弱的情况之下,大部分在1~3 m/s之间。500 m以下大气边界层内风速切变小,大气边界层内湍流强度不强,使沿海到内陆的逆温层能够始终维持,沿海海雾在弱南风影响下延伸影响内陆地区。     

超声波/声波钻头/取心器装置

目前,对宇宙中生命迹象的探索是世界各国所关注的最重要的目标之一。美国宇航局研制了由超声波或者声波驱动器驱动的一系列超声波/声波钻头/取心器（USDC）,用来进行空间探测并提取岩石、冰与土壤样品,以及进行原位分析。此设备在声波频率下,超声波压电驱动器驱动中间的自由质量块进而冲击钻头来进行采样。目前所制造的超声波钻头/取心器（USDC）装置能够取出岩心和岩屑,在未来的行星探测中,有着非常重要的优点。主要介绍USDC的优点、各装置的结构及其性能特点,以供我国月球探测工程及未来深空探测参考借鉴。     

High-resolution bispectrum speckle interferometry and two-dimensional radiative transfer modeling of the Red Rectangle

We present the first diffraction-limited K-band image of the Red Rectangle with 76 mas resolution, an H-band image with 75 mas resolution, and an RG 715 filter image ( 800 nm wavelength) with 78 mas resolution (corresponding to 25 AU for a distance of 330 pc). The H and K images were reconstructed from 6 m telescope speckle data and the RG 715 image from 2.2 m telescope data using the speckle masking bispectrum method. At all wavelengths the images show a compact, highly symmetric bipolar nebula, suggesting a toroidal density distribution of the circumstellar material. No direct light from the central binary can be seen as it is obscured by a dust disk or circumbinary torus. Our first high-resolution H−K color image of the nebula shows a broad red plateau of H−K≈ 2^m in the bright inner regions.The optical and near-infrared images and the available photometric continuum observations in a wide range of ultraviolet to centimeter wavelengths enabled us to model the Red Rectangle in detail using a two-dimensional radiative transfer code. Our model matches both the high-resolution images and the spectral energy distribution of this object very well, making the following picture much more certain. The central close binary system with a total luminosity of 3000 L is embedded in a very dense, compact circumbinary torus which has an average number density n_H ≈5×10¹² cm⁻³, an outer radius of the dense inner region of R≈30 AU (91 mas), and a ρ∝r⁻² density distribution. The full opening angle of the bipolar outflow cavities in our model is 70°. By comparing the observed and theoretical images, we derived an inclination angle of the torus to the line of sight of 7°±1°.The radiative transfer calculations show that the dust properties in the Red Rectangle are spatially inhomogeneous. The modeling confirms that the idea of large grains in the long-lived disk around the Red Rectangle (Jura et al., 1997 [ApJ, 474, 741]) is quantitatively consistent with the observations. In our models, unusually large, approximately millimeter-sized grains dominate the emission of the compact, massive torus. Models with smaller average grain sizes can possibly be found in future studies, for instance, if it turns out that the radio spectrum is not mainly caused by continuum dust emission. Therefore, the large grains suggested by our models require further confirmation by both new observations and radiative transfer calculations. Assuming a dust-to-gas ratio ρ_d/ρ_g of 0.005, the dense torus mass is 0.25 M. The model gives a lower limit of 0.0018 M, for the mass of the large particles, which produce a gray extinction of A≈ 28^m, towards the center. A much smaller mass of submicron-sized dust grains is presumably located in the polar outflow cavities, their conical surface layers, and in the outer low-density parts of the torus (where ρ∝r⁻⁴, in the region of 30 AUr 2000 AU corresponding to 0.^′′09–6^′′).     

X-ray absorption in the strong Fe ii narrow-line Seyfert 1 galaxy Markarian 507

We present results from spectral analysis of ASCA data on the strong Fe  ii narrow-line Seyfert 1 galaxy Mrk 507. This galaxy was found to have an exceptionally flat ROSAT spectrum among the narrow-line Seyfert 1 galaxies (NLS1s) studied by Boller, Brandt & Fink. The ASCA spectrum, however, shows a clear absorption feature in the energy band below 2 keV, which partly accounts for the flat spectrum observed with the ROSAT Position Sensitive Proportional Counter (PSPC). Such absorption is rarely observed in other NLS1s. The absorption is mainly the result of cold (neutral or slightly ionized) gas with a column density of (2–3) × 10²¹ cm⁻². A reanalysis of the PSPC data shows that an extrapolation of the best-fitting model for the ASCA spectrum underpredicts the X-ray emission observed with the PSPC below 0.4 keV if the absorber is neutral (which indicates that the absorber is slightly ionized), covers only part of the central source, or there is extra soft thermal emission from an extended region. There is also evidence that the X-ray absorption is complex; an additional edge feature marginally detected at 0.84 keV suggests the presence of an additional high-ionization absorber, which imposes a strong O  viii edge on the spectrum. After correction for the absorption, the photon index of the intrinsic continuum, Γ ≃ 1.8, obtained from the ASCA data is quite similar to that of ordinary Seyfert 1 galaxies. Mrk 507 still has one of the flattest continuum slopes among the NLS1s, but is no longer exceptional. The strong optical Fe  ii emission remains unusual in the light of the correlation between Fe  ii strengths and steepness of soft X-ray slope.     

The globular cluster system of the Sagittarius dwarf spheroidal galaxy: the age of Terzan 8

We present deep V - and I -band CCD photometry of the globular cluster Terzan 8, recently found to be a member of the globular cluster system of the Sagittarius dwarf spheroidal galaxy. We accurately estimate the metallicity of Terzan 8, and provide the first direct determination of the colour excess toward this cluster. Our robust age estimate confirms that this cluster is indeed coeval with typical Galactic globulars of comparable metal content, and thus it is probably significantly older than at least two other Sagittarius clusters, Terzan 7 and Arp 2. The implications of this result on the star formation history of the Sagittarius galaxy are briefly discussed.