REVIEWS OF GEOGRAPHIC SOFTWARE

Reviews of geographic software in this article: DEMO-GRAPHICS: WORLD POPULATIONS AND PROJECTIONS. ESP GAUSS. CEMODEL S. Damus LIMDEP. William H. Greene MICROSTAT 4.1 OTIS PCIPS. (Personal Computer Image Processing System) . H.J. Meyers and R. Bernstein. REGRESSION ANALYSIS OF TIME SERIES (RATS) SPSS/PC+ URBAN DATA MANAGEMENT SOFTWARE (UDMS)     

CAPPS多箱模式中光化学模式的嵌套与城市大气臭氧数值预报

为解决城市边界层中大气O₃浓度的预报问题，选用一种简明有效的光化学反应方案建立光化学模式, 并与大气平流扩散的箱格预报模型进行了嵌套，从而将大气化学过程引入到城市空气污染数值预报系统 (CAPPS) 中。同时，根据实际需要研究了VOC (Volatile Organic Compounds) 浓度及NO_x源排放量等参数缺测时，根据前期监测浓度采用遗传算法反演未知参数的具体方法。利用2001年9月8~17日在北京舞蹈学院监测的O₃、NO_x资料及相应的气象数据，用改进后的CAPPS模式进行了单箱预报试验。预报试验结果表明，嵌套后的模式对O₃浓度的变化具备一定的预报能力。     

基于Leica XPro系统的ADS80数字影像空三加密方法研究

ADS80航空摄影测量系统作为新一代的数字摄影系统,其获得的高分辨率航空影像已经广泛应用于我国各行业的基础建设项目中。Leica XPro系统是对ADS80影像数据做后续处理的主流软件之一,本文主要介绍了基于Leica XPro系统进行空三加密的流程,并对加密过程中可能遇到的一些问题加以分析和阐述。     

浅谈ADS100与ADS80航摄数据制作DOM的区别

随着摄影测量技术的发展,航摄影像的应用越来越广泛。本文针对目前应用较广泛的ADS80、ADS100相机在硬件组成、技术参数、利用像素工厂制作数字正射影像的区别进行了对比与分析,并探讨总结了生产正射影像过程中需要注意的问题,为今后的生产过程提供参考。     

2000国家大地坐标系椭球参数与GRS 80和WGS 84的比较

根据2000国家大地坐标系(CGCS 2000)的定义及其所定义的4个基本椭球常数,推导CGCS 2000椭球的主要几何和物理参数,比较这些参数与GRS 80和WGS 84椭球相应参数之间的差异,给出CGCS 2000椭球与GRS 80及WGS 84椭球定义的正常重力值的差异,并分析在CGCS 2000及WGS 84系下同一点坐标的差异.研究表明:CGCS 2000椭球上的正常重力值与GRS 80,WGS 84椭球上的正常重力值的差值分别约为-143.54×10-8m/s2和0.02×10-8m/s2.同一点在CGCS 2000与GRS 80和WGS 84下经度相同,纬度的最大差值分别为8.26×10-11"(相当于2.5×10-6 mm)和3.6×10-6"(相当于0.11 mm).     

Chlorinated hydrocarbons in gulls from the Baltic south coast

Polychlorinated terphenyls among organochlorine pesticides and polychlorinated biphenyls were detected in some gulls from the Gdańsk Bay, Baltic Sea.     

HST/STIS observations of the high-velocity interstellar cloud HVC 291.2−41.2+80: a warm, mainly ionized high-velocity cloud

We present intermediate-resolution HST /STIS spectra of a high-velocity interstellar cloud ( v _LSR=+80 km s⁻¹) towards DI 1388, a young star in the Magellanic Bridge located between the Small and Large Magellanic Clouds. The STIS data have a signal-to-noise ratio (S/N) of 20–45 and a spectral resolution of about 6.5 km s⁻¹ (FWHM). The high-velocity cloud absorption is observed in the lines of C  ii , O  i , Si  ii , Si  iii , Si  iv and S  iii . Limits can be placed on the amount of S  ii and Fe  ii absorption that is present. An analysis of the relative abundances derived from the observed species, particularly C  ii and O  i , suggests that this high-velocity gas is warm ( T _k∼10³–10⁴ K) and predominantly ionized. This hypothesis is supported by the presence of absorption produced by highly ionized species, such as Si  iv . This sightline also intercepts two other high-velocity clouds that produce weak absorption features at v _LSR=+113 and +130 km s⁻¹ in the STIS spectra.