天津市中心城区地下空间资源开发利用适宜性评价探讨

探讨了天津市中心城区的地下空间资源开发利用评价,提出了地下空间资源开发利用评价方法。分析了天津市中心城区的地质背景,论证选取了适宜的评价因子,结合目前中心城区地下空间的开发利用现状,对中心城区地下空间资源的开发利用进行了适宜性分区评价,为将来天津市中心城区地下空间资源的合理开发利用提出了建议。     

天津市潮间带柱状沉积物中重金属的污染历史及来源判别

利用因子分析和元素含量特征分析两种方法,对天津市潮间带的4个无扰动沉积物柱样的46个样品进行了重金属分析,并探讨了重金属的来源方式和富集原因。研究结果表明,天津市潮间带的重金属可分为3类:1)Fe、Cr、Al及Mn元素主要受环境背景值的影响,2)Hg和Cd受人为活动的影响较大,3)As、Zn、Pb、Cu及Ni受环境背景值及人类活动的双重影响,且影响大小随所在位置的不同而变化。结合210Pb和137Cs测年结果,定量确定了天津市潮间带小于0.063 mm粒级沉积物中Ni等11种重金属元素的环境背景值,并以此为基础,进一步探讨了重金属富集年代、富集量及污染历史和人类活动的关系,发现多数重金属的污染始于1910年代,并在1954年之后富集量增加。     

佛山市龙卷风活动的特征及环流背景分析

利用常规气象观测资料和NCEP再分析资料,分析了多年来佛山龙卷风的活动特点及其产生的环流背景和环境条件。结果表明:佛山龙卷风集中出现在4—8月;发生时间主要集中在08:00—14:00;发生地域以南海区最多,其次是三水区;16次龙卷风过程可归纳为4种诱生形势:台风外围型、锋面暖区型、地面辐合线型和热带扰动型。分析还发现:佛山龙卷风发生于偏南暖湿气流中,中低层通常有西南或偏南急流叠加配置,并存在强的垂直风切变和中干冷、下暖湿的强不稳定层结及较低的抬升凝结高度。另外,佛山龙卷风的发生还与地形因素关系密切。     

背景场和物理过程对WRF模式在新疆区域预报性能的影响

为了优选考虑新疆气候和地形特征的背景场和物理过程,设计WRF模式的Lin、WSM6、Thompson微物理过程和KF、Grell 3D积云参数化敏感性试验方案,使用T639和GFS两种背景场,进行了回算和对比检验,确定了在新疆预报能力最优的物理过程和背景场方案,并对WRF模式在新疆的预报能力和不足之处有了较为清晰的认识。     

江西德兴铜矿集区土壤地球化学基准值方法的适用性

确定矿集区土壤地球化学基准值是矿山环境地质调查与评价的重要任务,而遴选出合适的地球化学基线值的定值方法是该问题的关键。以江西德兴铜矿集区表层土壤地球化学数据为依据,运用地球化学对比法、相对累积频率方法和标准化的方法分别计算了德兴铜矿集区表层土壤6种重金属元素的地球化学背景值,并将其与江西省土壤背景值对比。结合成土母岩重金属含量分析了各种基准值定值方法的适用性,结果证明标准化方法较适用于确定研究区表层土壤地球化学基准值。     

Can the unresolved X-ray background be explained by the emission from the optically-detected faint galaxies of the GOODS project?

The emission from individual X-ray sources in the Chandra Deep Fields and XMM – Newton Lockman Hole shows that almost half of the hard X-ray background above 6 keV is unresolved and implies the existence of a missing population of heavily obscured active galactic nuclei (AGN). We have stacked the 0.5–8 keV X-ray emission from optical sources in the Great Observatories Origins Deep Survey (GOODS; which covers the Chandra Deep Fields) to determine whether these galaxies, which are individually undetected in X-rays, are hosting the hypothesized missing AGN. In the 0.5–6 keV energy range, the stacked-source emission corresponds to the remaining 10–20 per cent of the total background – the fraction that has not been resolved by Chandra . The spectrum of the stacked emission is consistent with starburst activity or weak AGN emission. In the 6–8 keV band, we find that upper limits to the stacked X-ray intensity from the GOODS galaxies are consistent with the ∼40 per cent of the total background that remains unresolved, but further selection refinement is required to identify the X-ray sources and confirm their contribution.     

The distribution of absorption in AGN detected in the XMM–Newton observations of the CDFS

We have used very deep XMM–Newton observations of the Chandra Deep Field -South to examine the spectral properties of the faint active galactic nucleus (AGN) population. Crucially, redshift measurements are available for 84 per cent (259/309) of the XMM–Newton sample. We have calculated the absorption and intrinsic luminosities of the sample using an extensive Monte Carlo technique incorporating the specifics of the XMM–Newton observations. 23 sources are found to have substantial absorption and intrinsic X-ray luminosities greater than 10⁴⁴ erg s⁻¹, putting them in the 'type-2' QSO regime. We compare the redshift, luminosity and absorption distributions of our sample to the predictions of a range of AGN population models. In contrast to recent findings from ultradeep Chandra surveys, we find that there is little evidence that the absorption distribution is dependent on either redshift or intrinsic X-ray luminosity. The pattern of absorption in our sample is best reproduced by models in which ∼75 per cent of the AGN population is heavily absorbed at all luminosities and redshifts.     

Bayesian foreground analysis with CMB data

The quality of CMB observations has improved dramatically in the last few years, and will continue to do so in the coming decade. Over a wide range of angular scales, the uncertainty due to instrumental noise is now small compared to the cosmic variance. One may claim with some justification that we have entered the era of precision CMB cosmology. However, some caution is still warranted: The errors due to residual foreground contamination in the CMB power spectrum and cosmological parameters remain largely unquantified, and the effect of these errors on important cosmological parameters such as the optical depth τ and spectral index n_s is not obvious. A major goal for current CMB analysis efforts must therefore be to develop methods that allow us to propagate such uncertainties from the raw data through to the final products. Here we review a recently proposed method that may be a first step towards that goal.     

Multi-Conjugate Adaptive Optics with laser guide stars: performance in the infrared and visible

The assumption of the Gaussianity of primordial perturbations plays an important role in modern cosmology. The most direct test of this hypothesis consists of testing the Gaussianity of cosmic microwave background (CMB) maps. Counting the pixels with the temperatures in given ranges and thus estimating the one-point probability function of the field is the simplest of all the tests. Other usually more complex tests of Gaussianity generally use a great deal of the information already contained in the probability function. However, the most interesting outcome of such a test would be the signal of non-Gaussianity independent of the probability function. It is shown that the independent information has purely morphological character i.e. it depends on the geometry and topology of the level contours only. As an example we discuss in detail the quadratic model   v = u + α ( u ²-1)  ( u is a Gaussian field with   u¯ =0  and  〈 u ²〉=1  , α is a parameter) that may arise in slow-roll or two-field inflation models. We show that in the limit of small amplitude α the full information about the non-Gaussianity is contained in the probability function. If other tests are performed on this model they simply recycle the same information. A simple procedure allowing us to assess the sensitivity of any statistics to the morphological information is suggested. We provide an analytic estimate of the statistical limit for detecting the quadratic non-Gaussianity α _c as a function of the map size in the ideal situation when the scale of the field is resolved. This estimate is in a good agreement with the results of the Monte Carlo simulations of 256² and 1024² maps. The effect of resolution on the detection quadratic non-Gaussianity is also briefly discussed.     

STUDIES ON ENVIRONMENTAL BACKGROUND VALUES IN CHINA

An investigation on environmental background values was made in an area of about 1,140,000 km2, which included temperate and subtropical zones of China. The environmental background values of 142 soil environment units, 18 main soil types, 87 surface water environment units, 8 aquatic organism environment units and 20 underground water environment units were obtained. The rules, causes and effecting factors of regional differentiation of the environmental background values were deduced from over 200,000 various data.