雷击地闪密度与雷暴日数的关系分析

根据美国卫星观测得到的我国各省区年平均总闪电资料并计算出各省区的年平均地闪密度(以下简称地闪密度);根据全国各省区220个站点的年平均雷暴日资料,按照<建筑物防雷设计规范>GB50057-94(2000年版)(以下简称<规范>)公式计算出全国各省区的地闪密度.比较两种方法得出的地闪密度,发现存在较大的差异,且不同区域差异变化很大.用单位雷暴日地闪密度概念,分析了我国各地单位雷暴日地闪密度的差异及其原因,指出单位雷暴日地闪密度能粗略反映与我国气候特征相适应的地闪密度的分布状况.进一步分析湖州市2007年人工观测和闪电定位仪观测的闪电资料,得到相同的结论.从而提出<规范>规定的地闪密度计算公式存在较大误差,应对其进行进一步的修订和完善.     

卫星微波被动遥感云中液态水的研究进展

卫星微波被动遥感云中液态水的研究在近30年中取得了较大的进展.卫星遥感仪器的不断进步、探测精度的不断提高为卫星微波被动遥感云中液态水提供了技术和资料保障,在此基础上针对卫星微波被动遥感云中液态水技术而发展的一些统计反演方法和物理反演方法不断地得到改进、完善和提高.文中主要就各个时期发展的主要反演方法做了简要回顾,概括了这些反演方法的关键技术,评述了各自的优点和局限性.由于海表和陆表的辐射特性的巨大差异,分别就海洋上空和陆地上空云中液态水的统计和物理反演技术方法进行了综述,并进行了比较.针对地表比辐射率这一制约陆地上空云中液态水反演技术发展的瓶颈问题,也进行了相关评述和讨论.     

Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D _* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star.     

Background studies for acoustic neutrino detection at the South Pole

The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500 m depth. The noise is very stable and Gaussian distributed. Lacking an in situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10-50 kHz frequency range to be smaller than 20 mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to test the localization of acoustic events. An upper limit on the neutrino flux at energies E_ν > 10¹¹ GeV is derived from acoustic data taken over eight months.     

绝对差分算法误差对测大气视宁度的影响分析

对绝对差分算法检测太阳边缘的起伏测量白日视宁度的方法进行了研究,并对绝对差分的结果进行二阶拟合使之可以达到亚像素的检测精度。对可能的影响因素如噪声和像差等进行了分析和数值模拟,算法的精度优于0．1”。模拟结果表明,采用绝对差分算法可以对白日视宁度进行高精度的测量,最后用绝对差分算法对实际数据进行了处理,给出了初步结果。     

Radio imaging of the Subaru/XMM–Newton Deep Field – II. The 37 brightest radio sources

We study the 37 brightest radio sources in the Subaru/ XMM–Newton Deep Field. We have spectroscopic redshifts for 24 of 37 objects and photometric redshifts for the remainder, yielding a median redshift z _med for the whole sample of   z _med≃ 1.1  and a median radio luminosity close to the 'Fanaroff–Riley type I/type II (FR I/FR II)' luminosity divide. Using mid-infrared (mid-IR) ( Spitzer MIPS 24 μm) data we expect to trace nuclear accretion activity, even if it is obscured at optical wavelengths, unless the obscuring column is extreme. Our results suggest that above the FR I/FR II radio luminosity break most of the radio sources are associated with objects that have excess mid-IR emission, only some of which are broad-line objects, although there is one clear low-accretion-rate object with an FR I radio structure. For extended steep-spectrum radio sources, the fraction of objects with mid-IR excess drops dramatically below the FR I/FR II luminosity break, although there exists at least one high-accretion-rate 'radio-quiet' QSO. We have therefore shown that the strong link between radio luminosity (or radio structure) and accretion properties, well known at z ∼ 0.1, persists to z ∼ 1. Investigation of mid-IR and blue excesses shows that they are correlated as predicted by a model in which, when significant accretion exists, a torus of dust absorbs ∼30 per cent of the light, and the dust above and below the torus scatters ≳1 per cent of the light.     

水资源全成本定价问题

随着经济的发展,人们对水资源的需求越来越多,水资源的天然供给与人类需求的矛盾越来越突出。在我国一些地区水资源不足已成为制约经济发展的一个主要瓶颈。但是一方面是水资源的不足,一方面又存在水资源的大量浪费,因此,合理配置水资源的使用已成为当务之急。配置资源的方式有2种,一种是计划手段,一种是经济手段,水资源的合理配置应将2种方法结合使用。文章依据马克思的劳动价值论,对水资源全成本定价方法进行了探讨。     

基于CSA-PLS算法的养殖水体水质快速高光谱预测反演模型研究

养殖水体水质的优劣直接影响养殖对象的成长,准确、快速、全面地掌控养殖水环境的水质参数变化情况具有重要意义。传统的水质指标监测方法都通过人工采样的方式,不仅耗费时间长,且只能体现局部水体情况。针对这些问题,提出了一种乌鸦搜索算法(CSA)结合偏最小二乘回归(PLSR)的高光谱特征波段筛选方法,快速构建回归模型,实现光谱数据的精准预测反演。以连片的养殖小区为研究对象,采集养殖水体样本并拍摄同时期的高光谱影像数据。首先对提取的采样点光谱数据利用多种数据变换方法分别预处理;其次利用这些数据,对水质指标总氮(TN)、氨氮(NH₄⁺-N)、总磷(TP)和化学需氧量(COD)分别构建全波段的SVR和AdaBoost回归模型,同时与提出的CSA-PLS自动筛选波段方法和传统的连续投影算法(SPA)筛选波段后构建的模型进行比较分析;最后根据决定系数(R²)和均方根误差(REMS)选出适合各水质指标的最优模型。从实验结果可以看出,所提波段筛选方法的AdaBoost模型预测结果优于SVR和传统SPA方法提取特征波段后构建的模型,与全波段最优模...     

地面稠密观测资料在强对流天气监测预警中的研究进展

综述国内外数篇论文,从强对流天气监测、预报预警、模式同化3个方面总结分析了近年来地面稠密观测资料的应用与优劣之处。综述表明:地面加密自动站、风廓线雷达、地基GPS、雨滴谱仪等多种观测仪器组成的地面稠密观测网具有时间尺度密集、覆盖面积广泛、能捕捉较多细微变化的优势,通过该观测网所得数据总结出的一系列指示性指标在强对流监测预警中具有重要的指示意义。但因中国地形天气情况复杂多变、数据缺失、仪器造价昂贵等问题,导致该观测网所得指示性指标不能适用于中国全境,应根据该观测网数据分析总结适应本地的预报指标。     

基于卫星高光谱遥感影像的浅海水深反演方法

遥感水深反演具有非接触测量和省时省力等优点,能够为航海、岛礁工程与珊瑚礁生态调查等活动提供重要参考。随着高光谱遥感卫星数量的增长,基于高光谱遥感影像的水深反演具有良好的发展与应用潜力。HOPE（Hyperspectral Optimization Process Exemplar）算法是比较常用的高光谱水深反演算法。鉴于HOPE算法在低遥感反射率海域会出现水深被高估的问题,本文基于Hyperion高光谱遥感影像提出一种改进的水深反演算法。该算法针对危险或难以到达海域往往具有水体光学性质较为均一的特点,利用深水区遥感反射率的观测值来估计整个研究区域内的水体光学性质参数并将其固定,以便减少未知参数数量,解决水深被高估的问题,最终达到提高水深反演整体精度的目的。塞班岛和中业岛的实验结果表明,改进算法能够有效克服常规HOPE算法在低遥感反射率水域高估水深的问题。改进算法能够将平均遥感反射率小于0.0075sr^-1（塞班岛）和0.001 sr^-1（中业岛）范围内的水域的水深反演平均绝对误差从常规HOPE算法的2.94 m和6.44 m分别降低至2.56 m和4.99 m,从而能够相应地将整体的均方根误差从3.18 m和5.39 m分别降低至2.30 m和3.32 m,而将整体的平均相对误差从32.4%和27.1%分别降低至30.6%和23.9%。因此,改进算法在提高卫星高光谱遥感影像水深反演效果方面具有可行性和有效性。