气象卫星遥感地表温度推算近地表气温方法研究   总被引：6，自引：0，他引：6  

韩秀珍  李三妹  窦芳丽 《气象学报》2012,70(5):1107-1118

气温是各种植物生理、水文、气象、环境等模式或模型中的一个非常重要的近地表气象参数.多年来气温数据以离散的常规气象站点观测为主,连续分布的格点气温数据则以站点资料插值而得到,分辨率低,无法反映地形等下垫面因素对局地气温的影响,在农业气候区划等研究中具有一定的局限性.随着卫星遥感地表温度算法的日趋成熟,为探讨卫星遥感地表温度数据在气温观测中的可能性和可行性,利用全中国2340个站点1998 2007年的逐旬平均最高气温数据,以及相应时段的NOAA/AVHRR旬最高地表温度数据,以线性回归及拟合模型为主,通过考虑植被指数、土地覆盖类型、季节、风速、气压、降水等各类影响因子,建立了旬最高地表温度与旬平均最高气温间的推算模型,并利用未参与建模的2002-2003年的常规气象站点气温数据,同时与推算气温和插值气温结果进行对比分析.结果表明,利用卫星遥感地表温度数据推算的旬值气温数据可取得较高的精度,尤其在地形复杂地区以及站点稀疏地区精度明显高于插值气温结果.  相似文献   

The Dynamical and Climate Tests of an Atmospheric General Circulation Model Using the Second-Order Adams-Bashforth Method          下载免费PDF全文

赵滨  钟青 《Acta Meteorologica Sinica》2009,23(6):738-749

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FGOALS_gg1.1极地气候模拟   总被引：4，自引：0，他引：4  

王秀成  刘骥平  俞永强  刘海龙  李立娟 《气象学报》2009,67(6)

对中国科学院大气物理研究所大气科学和地球流体力学数值模拟国家重点实验室发展的气候系统模式FGOALS_g1.1的极地气候模拟现状进行了较为全面的评估.结果表明,FGOALS_g1.1对南北极海冰的主要分布特征、季节变化和年代际变化趋势具有一定的模拟能力.但也注意到,与观测相比,模式存在以下几方面的问题:(1)模拟的海冰总面积北极偏多,而南极偏少.北极,北大西洋海冰全年明显偏多;夏季,西伯利亚沿海海冰偏多,而波弗特海海冰偏少.南极,威德尔海和罗斯海冬季海冰偏少.南北极海冰边缘都存在异常的较大范围密集度很小的碎冰区,夏季尤为显著.(2)海冰流速在南北极海冰边缘和南极大陆沿岸附近较大.北极,模式没能模拟出波弗特涡流,并且由于模式网格中北极点的处理问题,造成其附近错误的海冰流场及厚度分布.这些海冰偏差与模式模拟的大气和海洋状况有着密切的联系.进一步分析表明,FGOALS_g1.1模拟的冰岛低压和南极绕极西风带明显偏弱,其通过大气环流和海表面风应力影响向极地的热量输送,在很大程度上导致上述的海冰偏差.此外,耦合模式中大气-海冰-海洋的相互作用可以放大子模式中的偏差.  相似文献   

Wind measurements in Mars' middle atmosphere: IRAM Plateau de Bure interferometric CO observations     

R. Moreno  E. Lellouch  T. Encrenaz  E. Millour 《Icarus》2009,201(2):549-563

The IRAM Plateau de Bure Interferometer has been used to map the CO(1-0) rotational line in Mars' middle atmosphere. Absolute winds and thermal profiles were retrieved during the 1999, 2001, 2003 and 2005 planet's oppositions. The observations sampled various seasons (Ls=143, 196, 262, 317 and 322), and different dust situations (clear, global storm, regional storm). The absolute winds were derived by measuring directly the Doppler lineshifts. The main zonal circulation near 50 km is dominated by strong retrograde winds, with typical velocities of 70-170 m/s, strongly varying seasonally, latitudinally, and longitudinally (in particular between morning and evening). Comparison of the retrieved temperature with a general circulation model indicates that the model often underestimates the temperatures in the middle (20-50 km) atmosphere, and overestimates them above 50 km.  相似文献   

Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario     

J.-B. Madeleine  F. Forget  B. Levrard  E. Millour 《Icarus》2009,203(2):390-405

Recent geological observations in the northern mid-latitudes of Mars show evidence for past glacial activity during the late Amazonian, similar to the integrated glacial landsystems in the Dry Valleys of Antarctica. The large accumulation of ice (many hundreds of meters) required to create the observed glacial deposits points to significant atmospheric precipitation, snow and ice accumulation, and glacial flow. In order to understand the climate scenario required for these conditions, we used the LMD (Laboratoire de Météorologie Dynamique) Mars GCM (General Circulation Model), which is able to reproduce the present-day water cycle, and to predict past deposition of ice consistent with geological observations in many cases. Prior to this analysis, however, significant mid-latitude glaciation had not been simulated by the model, run under a range of parameters.In this analysis, we studied the response of the GCM to a wider range of orbital configurations and water ice reservoirs, and show that during periods of moderate obliquity (? = 25-35°) and high dust opacity (τ_dust = 1.5-2.5), broad-scale glaciation in the northern mid-latitudes occurs if water ice deposited on the flanks of the Tharsis volcanoes at higher obliquity is available for sublimation. We find that high dust contents of the atmosphere increase its water vapor holding capacity, thereby moving the saturation region to the northern mid-latitudes. Precipitation events are then controlled by topographic forcing of stationary planetary waves and transient weather systems, producing surface ice distribution and amounts that are consistent with the geological record. Ice accumulation rates of ∼10 mm yr⁻¹ lead to the formation of a 500-1000 m thick regional ice sheet that will produce glacial flow patterns consistent with the geological observations.  相似文献   

The jovian anticyclone BA: III. Aerosol properties and color change     

S. Pérez-Hoyos  A. Sánchez-Lavega  E. García-Melendo 《Icarus》2009,203(2):516-530

A study of the vertical cloud structure of oval BA and its red color change is presented in this third part of our complete analysis. A large interest in Jupiter’s anticyclone BA was created by its reddening that occurred between 2005 and 2006. In this work we quantify the color change in oval BA by using images taken with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST) in six filters from the near ultraviolet (F250W) to the deep methane band in the near infrared (F892N). Reflectivity changes are noteworthy in nadir viewing geometry at the ultraviolet and blue wavelengths (F250W, F330W and F435W filters) but almost undetectable or inside error bars in the rest of filters (F550M, F658N and F892N). The observed reflectivity variations are discussed in terms of a commonly accepted vertical cloud structure model for jovian anticyclones in order to explore some causes for the color alteration. Our models of the observed reflectivity variation show that the vortex clouds did not change its vertical extension (top pressure) or its optical depth. We find that a change occurred in the absorbing properties of the particles populating the upper aerosols (single scattering albedo and imaginary refractive index). A discussion on the thermo-physical and dynamical properties of the vortex that could be in the origin of the color change is also presented.  相似文献   

Spatial and short-term temporal variations in Uranus’ near-infrared spectrum     

J.W. Norwood  N.J. Chanover 《Icarus》2009,203(1):331-335

We obtained near-infrared spectra of Uranus at NASA’s Infrared Telescope Facility during the planet’s September 2006 and September 2007 oppositions. Ratios between the spectra indicate that in 2006, Uranus’ methane windows appeared much brighter in the south than in the north, and that between 2006 and 2007 they grew dimmer in the south and brighter in the north; we interpret these variations to be primarily caused by changing brightness in Uranus’ upper cloud layer near 2 bars.  相似文献   

First observation of CO at 345 GHz in the atmosphere of Saturn with the JCMT: New constraints on its origin     

T. Cavalié  F. Billebaud  M. Dobrijevic  T. Fouchet  T. Encrenaz  G.H. Moriarty-Schieven  P. Hartogh 《Icarus》2009,203(2):531-540

We have performed the first observation of the CO(3-2) spectral line in the atmosphere of Saturn with the James Clerk Maxwell Telescope. We have used a transport model of the atmosphere of Saturn to constrain the origin of the observed CO. The CO line is best-fit when the CO is located at pressures less than (15±2) mbar with a mixing ratio of (2.5±0.6)×10^-8 implying an external origin. By modeling the transport in Saturn’s atmosphere, we find that a cometary impact origin with an impact 200-350 years ago is more likely than continuous deposition by interplanetary dust particles (IDP) or local sources (rings/satellites). This result would confirm that comet impacts are relatively frequent and efficient providers of CO to the atmospheres of the outer planets. However, a diffuse and/or local source cannot be rejected, because we did not account for photochemistry of oxygen compounds. Finally, we have derived an upper limit of ∼1×10^-9 on the tropospheric CO mixing ratio.  相似文献   

大气折射与路径弯曲延迟     

童谞  萧耐园 《天文学报》2008,49(4)

电磁波信号在地球大气中的传播受到折射的影响,传播的方向发生了改变,传播的路径变为曲线,长度大于直线距离,相应的传播时间也被延长了,采用一个简化的球对称大气模型计算了光线在不同天顶距下由于路径弯曲而引起的延迟改正.  相似文献   

Coupling photochemistry with haze formation in Titan's atmosphere, Part II: Results and validation with Cassini/Huygens data     

P.P. Lavvas  A. Coustenis 《Planetary and Space Science》2008,56(1):67-99

The new one-dimensional radiative-convective/photochemical/microphysical model described in Part I is applied to the study of Titan's atmospheric processes that lead to haze formation. Our model generates the haze structure from the gaseous species photochemistry. Model results are presented for the species vertical concentration profiles, haze formation and its radiative properties, vertical temperature/density profiles and geometric albedo. These are validated against Cassini/Huygens observations and other ground-based and space-borne measurements. The model reproduces well most of the latest measurements from the Cassini/Huygens instruments for the chemical composition of Titan's atmosphere and the vertical profiles of the observed species. For the haze production we have included pathways that are based on pure hydrocarbons, pure nitriles and hydrocarbon/nitrile copolymers. From these, the nitrile and copolymer pathways provide the stronger contribution, in agreement with the results from the ACP instrument, which support the incorporation of nitrogen in the pyrolized haze structures. Our haze model reveals a new second major peak in the vertical profile of haze production rate between 500 and 900 km. This peak is produced by the copolymer family used and has important ramifications for the vertical atmospheric temperature profile and geometric albedo. In particular, the existence of this second peak determines the vertical profile of haze extinction. Our model results have been compared with the DISR retrieved haze extinction profiles and are found to be in very good agreement. We have also incorporated in our model heterogeneous chemistry on the haze particles that converts atomic hydrogen to molecular hydrogen. The resultant H₂ profile is closer to the INMS measurements, while the vertical profile of the diacetylene formed is found to be closer to that of the CIRS profile when this heterogenous chemistry is included.  相似文献