黑河中游荒漠绿洲农业适应气候变化技术研究   总被引：2，自引：0，他引：2       下载免费PDF全文

赵文智  杨荣 《气候变化研究进展》2010,6(3):204-209

以我国第二大内陆河流域——黑河流域的中游荒漠绿洲为例,基于长期定位试验成果,研究了绿洲农业适应气候变化的技术及其潜力。结果表明,在田间水平上,垄沟灌溉种植、主栽作物与伴生植物混播种植、优化水肥管理、建立枣粮复合系统是绿洲农业适应气候变化的有效技术;在绿洲水平上,调整农业种植结构、加大农田林网规格和减少农田林网的灌溉次数、降低防风固沙体系中高耗水树种——杨树的比例等技术是应对气候变化的重要途径。综合评价结果表明,在黑河中游绿洲,通过推广上述技术,在不降低绿洲农业产值和不影响绿洲生态系统稳定性的前提下,初步估算每年可节水2.96×108m3,抵消了气温上升大约1℃所带来的蒸散发消耗量。  相似文献   

湿热力平流参数在一次华北暴雨模拟诊断中的应用研究   总被引：1，自引：0，他引：1  

王成鑫  高守亭  梁钊明  梁莉 《气候与环境研究》2014,19(6):753-762

对2011年7月24~25日发生在华北地区的一次暴雨过程进行了分析,并以NCEP资料为初值场对此次暴雨过程进行了数值模拟,结合实况对模拟结果进行对比分析。分析表明:模式对本次华北暴雨的模拟比较成功,基本反映出了本次暴雨过程的降水分布特点。利用湿热力平流参数对本次华北地区的降水落区进行了诊断分析。分析指出,湿热力平流参数纬向平均的垂直剖面图上,湿热力平流参数的高值区及大值中心与地面的强降水雨区对应得较好,其梯度大小及向上延伸高度均可以定性地指示降水的强弱;垂直积分的湿热力平流参数与地面6 h强降水落区具有较好的对应关系,而在示踪弱降水区时效果并不是很好,其大值中心并不与强降水中心完全重叠,而是其梯度大值区与降水中心相对应;垂直积分的湿热力平流参数与6 h累积地面降水的空间分布特征和时间演变趋势比较相似,并且其变化趋势能反映降水的发展和消弱。  相似文献   

膜下条播冬麦栽培技术的进一步探讨     

艾尼瓦尔·依沙木丁 《沙漠与绿洲气象(新疆气象)》2008,2(2):46-48

膜下条播冬麦栽培技术是夺取旱地小麦和晚播小麦高产的一项突破性新技术,加之一次完成播种、铺膜一条龙播种机的配套高效作业,其增产显著。从膜下条播冬麦栽培技术在地区中试和示范3a来,使小麦生产上一个新台阶。  相似文献   

一次人工增雨作业中CA—FCM与其他评估方案的比较研究     

房彬  ;肖辉  ;班显秀  ;宫蔚蔚 《辽宁气象》2008,(4):13-18

根据2002年4月5日河南省人工催化增雨作业数据,分别采用作业区域趋势对比双比分析评估方案、区域趋势相关回归评估方案、区域趋势协变量多元回归评估方案、FCM（浮动对比区历史回归）评估方案、以降水量为协变量的CA—FCM评估方案和以降水量与整层大气可降水量为协变量的CA—FCM评估方案进行效果评估。结果表明：协变量由降水量和整层大气降水量2个组成的CA—FCM方法,由于引入了不受催化影响的物理协变量作为控制因子．以及采用了聚类分析提高了对比区和影响区相关性,其评估效果最好,显著水平高于0．05;其他评估方法评估效果较差。  相似文献   

黑龙江省年降水量和年平均气温序列均一性检验     

国世友  周振伟  侯兆滨 《黑龙江气象》2008,25(1):6-8

采用SNHT方法和台站历史沿革信息对黑龙江省62个地面观测站1961～2006年年降水量和年平均气温序列进行了均一性检验。结果表明：台站迁移、仪器更换等是造成黑龙江省年降水量序列非均一性的主要原因;年平均气温序列非均一性主要是由于仪器更换、台站迁移、观测时制变化等原因引起。  相似文献   

CHARACTERISTICS OF MEI-YU PRECIPITATION AND SVD ANALYSIS OF PRECIPITATION OVER THE YANGTZE-HUAIHE RIVERS VALLEYS AND THE SEA SURFACE TEMPERATURE IN THE NORTHERN PACIFIC OCEAN     

毛文书  王谦谦  彭骏  李永华 《热带气象学报(英文版)》2008,14(2):129-132

Based on the precipitation data of Meiyu at 37 stations in the valleys of Yangtze and Huaihe Rivers from 1954 to 2001, the temporal-spatial characteristics of Meiyu precipitation and their relationships with the sea surface temperature in northern Pacific are investigated using such methods as harmonic analysis, empirical orthogonal function (EOF), composite analysis and singular value decomposition (SVD). The results show that the temporal evolution and spatial distribution of Meiyu precipitation are not homogeneous in the Yangtze-Huaihe Rivers basins but with prominent inter-annual and inter-decadal variabilities. The key region between the anomalies of Meiyu precipitation and the monthly sea surface temperature anomalies (SSTA) lies in the west wind drift of North Pacific, which influences the precipitation anomaly of Meiyu precipitation over a key period of time from January to March in the same year. When the SST in the North Pacific west wind drift is warmer (colder) than average during these months, Meiyu precipitation anomalously increases (decreases) in the concurrent year. Results of SVD are consistent with those of composite analysis which pass the significance test of Monte-Carlo at 0.05.  相似文献   

基于RAMS/CFORS Ⅱ模式一次低空核试验放射性烟云扩散的数值模拟     

张彦  郑毅  王自发 《气候与环境研究》2008,13(6)

采用RAMS／CFORS Ⅱ模式模拟了一次低空核试验烟云的传输和沉降过程。CFORS Ⅱ模式是在RAMS／CFORS模式的基础上开发的,可用于对核试验放射性烟云长距离输送和沉降过程的模拟研究。模拟表明：对流层中低层的低压槽系统对本次低空核试验烟云的水平传输和垂直扩散起着重要的影响作用;烟云的长距离传输速度呈现出随高度递减而减小的趋势,在6000m以上,烟云在爆后48h即东移入海,6000m以下,烟云在中国大陆的扩散和沉降维持了5d以上;爆后2天内以大粒子沉降为主,其后以小粒子沉降为主,小粒子的放射性远小于大粒子,在爆后第4天,放射性沉降就减小了3个量级,而小粒子的沉降范围是大粒子的5倍以上。通过模拟和观测对比表明,模拟结果基本符合实际烟云的传输和沉降态势。  相似文献   

Atomic oxygen distribution in the Venus mesosphere from observations of O₂ infrared airglow by VIRTIS-Venus Express     

Jean-Claude Gérard  Adem Saglam  Pierre Drossart  Jean-Loup Bertaux 《Icarus》2009,199(2):264-272

This VIRTIS instrument on board Venus Express has collected spectrally resolved images of the Venus nightside limb that show the presence of the (0,0) band of the infrared atmospheric system of O₂ at 1.27 μm. The emission is produced by three-body recombination of oxygen atoms created by photodissociation of CO₂ on the dayside. It is consistently bright so that emission limb profiles can be extracted from the images. The vertical distribution of O₂() may be derived following Abel inversion of the radiance limb profiles. Assuming photochemical equilibrium, it is combined with the CO₂ vertical distribution to determine the atomic oxygen density. The uncertainties on the O density caused by the Abel inversion reach a few percent at the peak, increasing to about 50% near 120 km. We first analyze a case when the CO₂ density was derived from a stellar occultation observed with the SPICAV spectrometer simultaneously with an image of the O₂ limb airglow. In other cases, an average CO₂ profile deduced from a series of ultraviolet stellar occultations is used to derive the O profile, leading to uncertainties on the O density less than 30%. It is found that the maximum O density is generally located between 94 and 115 km with a mean value of 104 km. It ranges from less than 1×¹⁰¹¹ to about 5×¹⁰¹¹ cm⁻³ with a global mean of 2.2×¹⁰¹¹ cm⁻³. These values are in reasonable agreement with the VIRA midnight oxygen profile. The vertical O distribution is generally in good agreement with the oxygen profile calculated with a one-dimensional chemical-diffusive model. No statistical latitudinal dependence of the altitude of the oxygen peak is observed, but the maximum O density tends to decrease with increasing northern latitudes. The latitudinal distribution at a given time exhibits large variations in the O density profile and its vertical structure. The vertical oxygen distribution frequently shows multiple peaks possibly caused by waves or variations in the structure of turbulent transport. It is concluded that the O₂ infrared night airglow is a powerful tool to map the distribution of atomic oxygen in the mesosphere between 90 and 115 km and improve future Venus reference atmosphere models.  相似文献   

Titan at 3 microns: Newly identified spectral features and an improved analysis of haze opacity     

Haingja Seo  Joo Hyeon Kim  Régis Courtin 《Icarus》2009,199(2):449-457

We have reanalyzed the high-resolution spectrum of Titan between 2.87 and 3.12 μm observed with NIRSPEC/Keck II on 2001 Nov. 21 in southern summer, using updated CH₃D and C₂H₆ line-by-line models. From new synthetic spectra, we identify all but a few of the previously unidentified significant absorption spectral features in this wavelength range as due to these two species, both of which had been previously detected by Voyager and ground-based observations at other wavelengths. We also derive opacities and reflectivities of haze particles as functions of altitude for the 2.87-2.92 μm wavelength range, where Titan's atmosphere is partially transparent down to the surface. The extinction per unit altitude is observed to increase from 100 km (∼8 mbar) toward lower altitude. The derived total optical depth is approximately 1.1 for the 2.87-2.92 μm range. At wavelengths increasing beyond 2.92 μm the haze layers become much more optically thick, and the surface is rapidly hidden from view. These conclusions apply to equatorial and southern-temperate regions on Titan, excluding polar regions. We also find it unlikely that there is a large enhancement of the tropospheric CH₄ mole fraction over the value reported from analysis of the Huygens/GCMS observations.  相似文献   

Jupiter's hydrocarbon polar brightening: Discovery of 3-micron line emission from south polar CH₄, C₂H₂, and C₂H₆     

Sang J. Kim  T.R. Geballe  J.H. Kim 《Icarus》2009,202(1):354-357

Jupiter exhibits bright H⁺₃ auroral arcs at 3-4 microns that cool the hot (>1000 K) ionosphere above the ∼¹⁰−7 bar level through the infrared bands of this trace constituent. Below the ¹⁰−7 bar level significant cooling proceeds through infrared active bands of CH₄, C₂H₂, and C₂H₆. We report the discovery of 3-micron line emission from these hydrocarbon species in spectra of the jovian south polar region obtained on April 18 and 20, 2006 (UT) with CGS4 on the United Kingdom Infrared Telescope. Estimated cooling rates through these molecules are 7.5×¹⁰−3, 1.4×¹⁰−3, and , respectively, for a total nearly half that of H⁺₃. We derive a temperature of 450 ± 50 K in the ¹⁰−7-¹⁰−5 bar region from the C₂H₂ lines.  相似文献