利用地面激光扫描数据进行建筑物变化检测

利用地面激光扫描仪具有的数据获取速度快、精度高、实时性强、能全天候工作等优点,在快速获取三维点云的基础上,通过点云自动拼接、Hausdorff距离检测不同时期建筑物的三维模型变化,并改进了检测算法,提高了算法的执行效率。通过拟合平面构建Delaunay三角网求解变化区域的面积来评估灾害对建筑物的破坏程度,从而为灾害应急响应以及保险理赔等提供了可靠的决策依据。     

云凝结核浓度对不同弗罗德数下形成的地形云和降水的影响

云凝结核(CCN)对云和降水的影响除与其物理化学性质密切相关外,还受到气象条件的影响,但此类研究较少。文中基于WRF中尺度数值模式,引入了表征大气层流速、层结稳定度和地形关系的湿弗罗德(Fw)数,研究揭示了CCN浓度的变化对不同Fw下形成的地形云和降水的影响。研究表明,当Fw≤1,接近临界流时,地形阻挡起主要作用,地形抬升和重力波作用主要发生在迎风坡一侧,主要形成层状云和向上游传播的浅对流波状云,降水主要发生在靠近山顶的迎风坡一侧。在此种情况下,CCN浓度升高对地形云和降水影响较小,当CCN浓度由100 cm~(-3)增至1000 cm~(-3)时,云滴含水量增大,但雨水含量减小,说明云粒子向降水粒子的转化效率降低,CCN浓度升高抑制了暖雨过程。但在云发展后期,云滴被上升气流带至高层形成过冷云滴,与雪粒子发生碰并形成霰粒子,使冰相物理过程有所增强。CCN浓度升高可导致20 h累积降水量减少10—15 mm,约减小7%—8%;当Fw1时,CCN浓度升高会导致20 h地形云累积降水量减小超过50%,最大达到96%,导致地形云几乎不产生降水,而且降水量峰值位置向山顶后移动5—10 km。研究表明,降水显著减小的原因不仅与CCN浓度升高有关,过山气流产生的背风坡焚风效应也起了非常重要的作用。由于CCN浓度升高形成了大量云滴粒子,使雨滴形成效率显著降低,不能形成降雨的大量云滴被强过山气流快速带至下游背风坡区,由于背风坡下坡气流的绝热加热形成的焚风效应很显著,导致云滴和雨滴快速蒸发,使降水显著减小。这一结果可以解释在落基山脉、以色列及中国华山发现的地形降水减小30%—50%的现象,说明气象环境条件在气溶胶影响降水中起重要作用,污染气溶胶与背风坡焚风效应产生的叠加效应可造成地形云降水显著减小。     

“碧利斯”(0604)暴雨过程不同类型降水云微物理特征分析

本文利用"碧利斯"(0604)暴雨增幅过程高分辨率的数值模拟资料, 将降水分成对流降水和层云降水, 对比分析了不同类型降水云微物理特征和过程的差异, 探讨了不同类型降水对暴雨增幅的贡献, 结果指出:(1)暴雨增幅前, 降水基本为层云降水, 对流降水只存在于零星的几个小区域, 暴雨增幅发生时段, 对流降水所占比例较暴雨增幅前有显著增加, 平均降水强度达层云降水强度的3倍多。(2)暴雨增幅时段, 云系发展更加旺盛, 云中各种水凝物含量较增幅前明显增加, 其中, 对流和层云降水区云中水凝物含量均有一定程度增长, 但对流降水区增加更显著;而无论增幅前还是增幅时段, 对流降水区云中水凝物含量均要明显大于层云降水区, 并且两者的这种差异随着地面降水强度的增强而增大。(3)暴雨增幅前后, 对流降水区雨滴的两个主要来源最终均可以追踪到云水, 通过云水与大的液相粒子(雨滴)和大的固相粒子(雪)之间、以及大的固相粒子(雪和霰)之间的相互作用和转化, 造成雨滴增长, 并最终形成地面降水, 而层云降水区中与雨滴形成相关的上述主要云微物理过程明显变弱, 但层云降水区中暴雨增幅时段的上述过程又要强于增幅前, 说明层云降水对暴雨增幅也有一定贡献。     

Hα emission objects in Circinus

We present a new survey for Hα emission objects in the Circinus cloud complex and introduce an efficient photometric method for detecting Hα emission via observations in a narrow‐band filter. The observed flux is compared to a blackbody fit of the continuum. Our search strategy reveals 20 stars with strong Hα emission (EW > 10 Å), eight of them being new detections. All Hα stars display infrared excess corroborating their youth. On the other hand, the region contains a number of infrared excess objects that do not show Hα emission. Our results support the picture that accretion – as witnessed by Hα emission – is a highly variable phenomenon. Therefore, Hα surveys can only trace the temporarily active objects. In contrast, infrared excess is a more robust tracer that reveals most of the population of young stellar objects in a star forming region. Our analysis of the general stellar content of the region yields a reliable distance of 450 pc for the Circinus cloud. Moreover, we find a ratio of total‐to‐selective extinction of R^V = 2.8 suggesting that smaller‐than‐normal dust grains may be present. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

J1128+592: a highly variable IDV source

Short time‐scale radio variations of compact extragalactic radio quasars and blazars known as IntraDay Variability (IDV) can be explained in at least some sources as a propagation effect; the variations are interpreted as scintillation of radio waves in the turbulent interstellar medium of the Milky Way. One of the most convincing observational arguments in favor of a propagation‐induced variability scenario is the observed annual modulation in the characteristic time scale of the variation due to the Earth's orbital motion. So far there are only two sources known with a well‐constrained seasonal cycle. Annual modulation has been proposed for a few other less well‐documented objects. However, for some other IDV sources source‐intrinsic structural variations which cause drastic changes in the variability time scale were also suggested. J1128+592 is a recently discovered, highly variable IDV source. Previous, densely time‐sampled flux‐density measurements with the Effelsberg 100‐m radio telescope (Germany) and the Urumqi 25‐m radio telescope (China), strongly indicate an annual modulation of the time scale. The most recent 4 observations in 2006/7, however, do not fit well to the annual modulation model proposed before. In this paper, we investigate a possible explanation of this discrepancy. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Cloud drop spectra at different levels and with respect to cloud thickness and rain

Measurements on drop size were made in cumulus clouds over Pune (inland region) during the summer monsoon seasons. In this paper, the measurements of the cloud drop spectra made in non-raining clouds at different levels and for different thickness have been studied. Also, those on the days with rain and with no rain (the rain being observed within the clouds) have been compared. The average spectra broadened with height. The concentration of drops >50 μm (N_L), liquid water content (LWC), mean volume diameter (MVD) and dispersion increased with height. The concentration of drops <20 μm (N_S) and total concentration (N_T) decreased with height. The spectra were broader, while N_S and N_T are smaller and the other parameters are greater for thicker clouds as compared to those for thinner. The spectra were broader, while N_S and N_T are smaller and the other parameters are greater on the days with rain with respect to those on the days with no rain. The distributions were bimodal at higher levels, for thicker clouds and on the days with rain, while they were unimodal at lower levels, for thinner clouds and on the days with no rain. The variations of the cloud drop spectra, preceding rain, at initial stage of rain and following rain are discussed.     

Study on horizontal relative diffusion in the troposphere and lower stratosphere

The behaviour of relative diffusion theory and Gifford’s random-force theory for long-range atmospheric diffusion is examined. When a puff scale is smaller than the Lagrangian length scale, 2KTL, an accelerative relative diffusion region exists, i.e., σy∝t3/2. While the puff diffusion enters a two-dimensional turbulence region, in which the diffusion scale is larger than 500 km, or time scale is larger than 1 day, divergence and convergence are main cause of horizontal diffusion. Between the two above-mentioned regimes, diffusion deviation is given byσy=2KTL. The large-scale horizontal relative diffusion parameters were obtained by analyzing the data of radioactive cloud width collected in air nuclear tests.     

New models of interstellar gas–grain chemistry – I. Surface diffusion rates

In recent years it has become evident that large differences can exist between model results of grain-surface chemistry obtained from a rate equation approach and from a Monte Carlo technique. This dichotomy has led to the development of a modified rate equation method, in which a key element is the artificial slowing down of the diffusion rate of surface hydrogen atoms. Recent laboratory research into the surface diffusion rate of atomic hydrogen suggests that atomic hydrogen moves more slowly on grains than heretofore assumed. This research appears to lessen the need for modifications to the rate equation method. Based on the new laboratory work, we have developed appropriate models of gas-phase and grain-surface chemistry in quiescent dense cloud cores to examine the chemical effects of slowing down the rate at which atomic H can scan over dust surfaces. Furthermore, we have investigated the effect of slowing down the rate at which all species can move over grain surfaces.     

Interstellar CO towards X Persei (HD 24534) – II. Two-component model

The observations made by the Goddard High Resolution Spectrograph (GHRS) aboard the Hubble Space Telescope ( HST ) of molecular CO in absorbing gas towards X Persei are reported. The two-component statistical equilibrium model incorporating radiative excitation of CO by line emission at the same velocity that originates in nearby molecular clouds has been used to reproduce high-resolution GHRS spectra. Earlier analysis indicates that the cloud has a complex structure and at least a two-component model should be used to obtain accurate results. The spectra obtained from the International Ultraviolet Explorer ( IUE ) were used to complement GHRS data and constrain the space of possible solutions. The new oscillator strengths recommended by Eidelsberg et al. for A–X bands have been used. The results show that one of the components may be attributed to the Perseus OB2 molecular cloud, and the other component to an extension of the Taurus dark cloud. The total CO column density N (CO)=(1.0±0.2)×10¹⁶ cm⁻² has been determined. According to the results about 85 per cent of the observed CO belongs to an extension of the Taurus dark cloud. The CO radiation that originates in nearby molecular clouds may be the dominant excitation mechanism of the observed CO. The early results of ¹³CO line analysis indicate a ¹³CO/¹²CO ratio of about 40.