一种高频雷达回波谱反演海浪的新算法

在高频地波雷达海浪谱反演问题中,广泛采用的Barrick后向散射公式属于第一类非线性Fredholm积分方程。此类积分方程的解在本质上是不适定的,加之高频雷达二阶回波信号信噪比较低,使得反演海浪谱存在解不稳定的问题。本文提出一种稳定且低复杂度的反演算法,此算法首先根据高频雷达一阶回波谱测量海浪方向,并将其引入积分方程求解过程,减少求解变量的个数,降低反演算法的复杂度。为解决反演结果不稳定的问题,使用Tikhonov正则化方法并利用广义交叉验证法(GCV)确定其正则化系数。通过在不同测试条件下对反演算法的仿真测试分析,表明此方法具有运算量小、稳定性好的特点。     

Radar altimetry backscattering signatures at Ka,Ku, C,and S bands over West Africa

This study presents a comprehensive comparison of radar altimetry signatures at Ka-, Ku-, C-, and S-bands using SARAL, ENVISAT and Jason-2 data over the major bioclimatic zones, soil and vegetation types encountered in West-Africa, with an emphasis on the new information at Ka-band provided by the recently launched SARAL–Altika mission. Spatio-temporal variations of the radar altimetry responses were related to changes in surface roughness, land cover and soil wetness. Analysis of time series of backscattering coefficients along the West African bioclimatic gradient shows that radar echoes at nadir incidence are well correlated to soil moisture in semi-arid savannah environments. Radar altimeters are able to detect the presence of water even under a dense canopy cover at all frequencies. But only measurements at Ka-band are able to penetrate underneath the canopy of non-inundated tropical evergreen forests.     

The variability of Mercury's exosphere by particle and radiation induced surface release processes

Mercury's close orbit around the Sun, its weak intrinsic magnetic field and the absence of an atmosphere (P_surface<1×10⁻⁸ Pa) results in a strong direct exposure of the surface to energetic ions, electrons and UV radiation. Thermal processes and particle-surface-collisions dominate the surface interaction processes leading to surface chemistry and physics, including the formation of an exosphere (N?10¹⁴ cm⁻²) in which gravity is the dominant force affecting the trajectories of exospheric atoms. NASA's Mariner 10 spacecraft observed the existence of H, He, and O in Mercury's exosphere. In addition, the volatile components Na, K, and Ca have been observed by ground based instrumentation in the exosphere. We study the efficiency of several particle surface release processes by calculating stopping cross-sections, sputter yields and exospheric source rates. Our study indicates surface sputter yields for Na between values of about 0.27 and 0.35 in an energy range from 500 eV up to 2 keV if Na⁺ ions are the sputter agents, and about 0.037 and 0.082 at an energy range between 500 eV up to 2 keV when H⁺ are the sputter agents and a surface binding energy of about 2 eV to 2.65 eV. The sputter yields for Ca are about 0.032 to 0.06 and for K atoms between 0.054 to 0.1 in the same energy range. We found a sputter yield for O atoms between 0.025 and 0.04 for a particle energy range between 500 eV up to 2 keV protons. By taking the average solar wind proton surface flux at the open magnetic field line area of about 4×10⁸ cm⁻² s⁻¹ calculated by Massetti et al. (2003, Icarus, in press) the resulting average sputtering flux for O is about 0.8-1.0×10⁷ cm⁻² s⁻¹ and for Na approximately 1.3-1.6×10⁵ cm⁻² s⁻¹ depending on the assumed Na binding energies, regolith content, sputtering agents and solar activity. By using lunar regolith values for K we obtain a sputtering flux of about 1.0-1.4×10⁴ cm⁻² s⁻¹. By taking an average open magnetic field line area of about 2.8×10¹⁶ cm² modelled by Massetti et al. (2003, Icarus, in press) we derive an average surface sputter rate for Na of about 4.2×10²¹ s⁻¹ and for O of about 2.5×10²³ s⁻¹. The particle sputter rate for K atoms is about 3.0×10²⁰ s⁻¹ assuming lunar regolith composition for K. The sputter rates depend on the particle content in the regolith and the open magnetic field line area on Mercury's surface. Further, the surface layer could be depleted in alkali. A UV model has been developed to yield the surface UV irradiance at any time and latitude over a Mercury year. Seasonal and diurnal variations are calculated, and Photon Stimulated Desorption (PSD) fluxes along Mercury's orbit are evaluated. A solar UV hotspot is created towards perihelion, with significant average PSD particle release rates and Na fluxes of about 3.0×10⁶ cm⁻² s⁻¹. The average source rates for Na particles released by PSD are about 1×10²⁴ s⁻¹. By using the laboratory obtained data of Madey et al. (1998, J. Geophys. Res. 103, 5873-5887) for the calculation of the PSD flux of K atoms we get fluxes in the order of about 10⁴ cm⁻² s⁻¹ along Mercury's orbit. However, these values may be to high since they are based on idealized smooth surface conditions in the laboratory and do not include the roughness and porosity of Mercury's regolith. Further, the lack of an ionosphere and Mercury's small, temporally and spatially highly variable magnetosphere can result in a large and rapid increase of exospheric particles, especially Na in Mercury's exosphere. Our study suggests that the average total source rates for the exosphere from solar particle and radiation induced surface processes during quiet solar conditions may be of the same order as particles produced by micrometeoroid vaporization. We also discuss the capability of in situ measurements of Mercury's highly variable particle environment by the proposed NPA-SERENA instrument package on board ESA's BepiColombo Mercury Planetary Orbiter (MPO).     

向心扩张指数构建及其在郑州都市圈城镇空间扩张中的应用

探究城镇空间扩张的方向性及其时间变化特征,能够反映都市圈发展过程中核心城市与边缘地区空间关联的动态过程,为制定都市圈发展的相关政策提供科学依据。本文从都市圈的核心城市与边缘地区相互关联的视角,借鉴物理学中力的分解原理,构建了同时兼顾扩张强度和方向性的向心扩张指数CEI,并以郑州都市圈为对象,采用2000—2018年30 m分辨率的全球人造不透水面数据产品GAIA,分析了建设用地扩张的总体数量和占比变化、动态度及强度变化、以及空间方向性变化等特征,进一步应用多元逻辑回归模型,揭示了影响城镇空间扩张向心性的关键因素。结果表明：(1)向心扩张指数CEI为揭示都市圈核心城市对边缘地区的辐射带动作用提供方法支撑,能够定量刻画边缘地区朝向核心城市的发展趋势;(2)在郑州都市圈近20年的快速扩张过程中,尽管各区县市的DEI指数和CEI指数随时间而增减波动,但郑州都市圈总体呈现“核心—边缘”发展模式,除个别地级市中心城区及其下辖县以外,多数区县市的向心性显著且随时间增强,郑州市中心城区对于边缘地区具有显著的辐射带动作用;(3)核心城市与边缘地区的人均GDP差异及城镇化率差异是影响边缘地区向心扩张的重要...     

城市生活垃圾卫生填埋场沉降变形分析

城市生活垃圾填埋场地基沉降和垃圾堆体沉降受到的影响因素多,现行规范的计算方法直接采用与实际相差较大,为减少不均匀沉降对垃圾防渗层的影响、准确确定垃圾储量和保证垃圾堆体的稳定,开展垃圾填埋场沉降研究具有重要意义。垃圾填埋场沉降变形包括地基沉降和垃圾堆体沉降,垃圾堆体沉降又分为主沉降和次沉降,主沉降完成时间短于次沉降。通过对陕西省宝鸡市垃圾填埋场地基土进行沉降计算,最大沉降差超过100 mm,对垃圾防渗层不利影响较大;而对垃圾堆体沉降计算,修正后的计算值与沉降观测值非常接近。考虑不同地区地层差异和垃圾成分差异,积累沉降观测资料具有重要意义。     

水流注入方式和填料层高度对人工湿地流态的影响

流态模拟实验作为评价人工净化湿地系统运行状况、物质在其中停留时间的有效工具,在污水处理领域具有重要作用。罗丹明B背景浓度低、重现性好,被选为评价升流式、降流式和填料层高度对水力流态影响的示踪剂。实验使用罗丹明B和NaCl作为示踪剂,在湿地系统中进行流态实验,探究升流式、降流式和填料层高度对人工净化湿地流态的影响。实验结果表明,升流式人工湿地比降流式人工湿地处理效果好,示踪剂水力停留时间(hydraulic retention time,HRT)的体积利用率分别为82.0%和76.8%,升流式人工湿地无效体积中死区占更大比例,而降流式人工湿地滞留区占无效体积的比例更大;人工湿地填料层高度对示踪剂停留时间分布影响不大,体积利用率都在80%以上,但是,其死区和滞留区随着填料层高度的变化在无效体积中所占的比例有所差异,死区所占的比例随着填料层高度的增加先增加后减少,滞留区所占的比例则先减少后增加。     

Daily variability of dissolved inorganic radiocarbon at three sites in the surface ocean

We report radiocarbon measurements of dissolved inorganic carbon (DIC) in surface water samples collected daily during cruises to the central North Pacific, the Sargasso Sea and the Southern Ocean. The ranges of Δ¹⁴C measurements for each cruise (11–30‰) were larger than the total uncertainty (7.8‰, 2-sigma) of the measurements. The variability is attributed to changes in the upper water mass that took place at each site over a two to four week period. These results indicate that variability of surface Δ¹⁴C values is larger than the analytical precision, because of patchiness that exists in the DIC Δ¹⁴C signature of the surface ocean. This additional variability can affect estimates of geochemical parameters such as the air–sea CO₂ exchange rate using radiocarbon.     

一种改进的数值预报降水偏差订正方法及应用

对传统的消除偏差法进行改进,形成分等级消除偏差法,并使用混合训练期和60 d滑动训练期方案分别对2012年6—8月ECMWF (European Centre for Medium-Range Weather Forecasting) 模式夏季1~5 d的降水预报进行订正试验。为了尽可能符合中国东部夏季降水具有移动性及多种时间尺度变化的特点,混合训练期以预报期前30 d与预报期前一年同日的前后各15 d组成。结果表明:在使用分等级消除偏差法的基础上,相比ECMWF模式降水预报,两种训练期方案的订正结果几乎对各个阈值的ETS评分均有一定提高,特别是对25 mm以上降水预报评分的提高幅度,混合训练期方案的订正结果明显高于60 d滑动训练期方案;在区域性强降水预报的订正中,混合训练期方案优势更为明显。另外,通过分析两种训练期方案的预报偏差发现,分等级订正是此次消除偏差订正试验中提高强降水预报评分的关键,选择合适的训练期可以增加评分提高的幅度。由于上述试验使用的ECMWF模式预报和站点实况均是业务上常用数据,因此,该方法具有一定的业务应用价值。     

The surface composition of Trojan asteroids: constraints set by scattering theory

We present the results of spectral modeling of 17 Trojan asteroids. The surface composition of this group of objects (located just beyond the main belt, trapped in Jupiter's stable Lagrange points) remains uncertain due to an absence of diagnostic absorption features in their spectra. We quantitatively analyze spectra of these objects covering the range 0.3-4.0 μm using the formulation for scattering in a particulate medium developed by Hapke. Since the widest spectral range possible is desired to provide the most robust results, recently measured near-IR spectra are combined with previously published visible and near-IR data. These composite spectra are converted to and modeled in terms of geometric albedo to provide the additional constraint of the absolute brightness of the asteroids. It is important that this modeling is performed for a large number of objects, and results are derived based on trends among best-fit models. Under this rigorous examination, we find that it is unlikely that the red spectral slope is a result of organics on the surfaces, due mainly to the lack of absorptions in the L-band. Instead, anhydrous silicates adequately describe the spectral characteristics of this group of objects. A significant fraction of carbonaceous material is also likely present, but is not responsible for the red spectral slope in these models. Also, using these models, we estimate that these surfaces contain at most a few wt% of H₂O ice and no more than 10-30 wt% of hydrated silicates.     

铁路碎石道碴层通风阻力参数试验研究

铁路碎石道碴层能被看作高渗透率的多孔介质,由于其具有较好的通风特性,它的存在改变了寒区铁路路基的顶部热交换条件,对路基温度场产生不可忽视的影响.为了能够实现对寒区铁路路基温度场的更合理预测,基于对铁路碎石道碴层传热和通风特性的研究现状,通过风洞试验对铁路碎石道碴层的通风特性及通风阻力参数进行了试验研究.试验中选用的铁路碎石道碴平均粒径为4.2cm,孔隙率为0.433,对不同空洞风速条件下铁路碎石道碴层中的压力梯度和渗流速度进行了测试分析.结果表明:铁路碎石道碴层中空气渗流速度随着压力梯度的增大而增大,其内部压力梯度与渗流速度之间存在良好的二次非线件关系.通过计算得到铁路碎石道碴层的渗透率和惯性阻力系数,为寒区铁路路基热稳定性的数值研究提供了参数依据.