中国大气本底观测发展概述   总被引：1，自引：0，他引：1  

李伟 孙扬程根伟  王可琴李同阳 刘发蓉 《山地学报》2006,24(B10):324-329

中国早期的大气本底观测网建设起步于上世纪80年代初，并于10a后基本建成。目前，中国气象局、中国科学院在原有观测站的基础上各自建设和发展着自己下属的大气本底观测网络。全球大气观测网给出了一整套开展大气本底观测的技术标准，各国均予以严格遵循。20多年来，中国大气本底观测工作在基础数据积累以及观测标准制定等方面取得了较大进展，与此相关的科学研究也取得了长足进步。最后对中国大气本底观测发展过程中存在的一些问题进行了探讨。  相似文献   

2004年春季中国沙尘天气特征分析          下载免费PDF全文

周自江  牛若芸 《气象科学》2007,27(1):69-75

利用全国681个站的沙尘天气观测资料分析得出,2004年春季中国北方的沙尘天气明显偏少、偏弱,主要表现在：（1）2004年春季681个站累计的沙尘天气日数2 080 d,相当于历史平均值的46.9%,是近四十余年中第三个偏少年份。沙尘暴的总面积约190万km2,仅为历史平均值的37.3%。（2）危害性较大的沙尘暴和强沙尘暴过程6次,不足2001年的一半。（3）4月和5月沙尘天气明显偏少导致整个春季显著偏少。沙尘天气出现时,PM10浓度相对增加,空气质量恶化,但与历史上较典型的强沙尘暴个例相比,PM10浓度增加的幅度不大。进一步分析表明,2004年春季沙尘天气偏少、偏弱的主要原因是大气动力条件不足,是比较特殊的一个年份。  相似文献   

一种快速地球大气效果3维绘制方法     

LAN Chao-zhen  LI Jian-sheng  XU Qin 《测绘学院学报》2007,(Z1)

介绍了地球大气模型,并回顾了国内外大气的3维绘制算法。在此基础上提出了一种基于简化模型的快速大气效果绘制算法。该算法综合利用Billboard与图形学雾化效果,逼真模拟出了地球大气的可视化效果。实验结果表明,该算法简单有效,避免了复杂的物理计算,大大提高了绘制效率。  相似文献   

Role of H₂O and CO₂ Ices in Martian Climate Changes     

Tokuta YokohataMasatsugu Odaka  Kiyoshi Kuramoto 《Icarus》2002,159(2):439-448

In order to study the stability of martian climate, we constructed a two-dimensional (horizontal-vertical) energy balance model. The long-term CO₂ mass exchange process between the atmosphere and CO₂ ice caps is investigated with particular attention to the effect of planetary ice distribution on the climate stability. Our model calculation suggests that high atmospheric pressure presumed for past Mars would be unstabilized if H₂O ice widely prevailed. As a result, a cold climate state might have been achieved by the condensation of atmospheric CO₂ onto ice caps. On the other hand, the low atmospheric pressure, which is buffered by the CO₂ ice cap and likely close to the present pressure, would be unstabilized if the CO₂ ice albedo decreased. This may have led the climate into a warm state with high atmospheric pressure owing to complete evaporation of CO₂ ice cap. Through the albedo feedback mechanisms of H₂O and CO₂ ices in the atmosphere-ice cap system, Mars may have experienced warm and cold climates episodically in its history.  相似文献   

CO₂ Snow on Mars and Early Earth: Experimental Constraints     

David L. GlandorfAnthony Colaprete  Margaret A. TolbertOwen B. Toon 《Icarus》2002,160(1):66-72

Greenhouse warming due to carbon dioxide atmospheres may be responsible for maintaining the early Earth's surface temperature above freezing and may even have allowed for liquid water on early Mars. However, the high levels of CO₂ required for such warming should have also resulted in the formation of CO₂ clouds. These clouds, depending on their particle size, could lead to either warming or cooling. The particle size in turn is determined by the nucleation and growth conditions. Here we present laboratory studies of the nucleation and growth of carbon dioxide on water ice under martian atmospheric conditions. We find that a critical saturation, S=1.34, is required for nucleation, corresponding to a contact parameter between solid water and solid carbon dioxide of m=0.95. We also find that after nucleation occurs, growth of CO₂ is very rapid, and we report the growth rates at a number of supersaturations. Because growth would be expected to continue until the CO₂ pressure is lowered to its vapor pressure, we expect particles larger than those being currently suggested for the present and past martian atmospheres. Using this information in a microphysical model described in a companion paper, we find that CO₂ clouds are best described as “snow,” having a relatively small number of large particles.  相似文献   

Monte Carlo Radiative Transfer Modeling of Lightning Observed in Galileo Images of Jupiter   总被引：1，自引：0，他引：1  

U.A. DyudinaA.P. Ingersoll  A.R. VasavadaS.P. Ewald  the Galileo SSI Team 《Icarus》2002,160(2):336-349

We study lightning on Jupiter and the clouds illuminated by the lightning using images taken by the Galileo orbiter. The Galileo images have a resolution of ∼25 km/pixel and are able to resolve the shape of single lightning spots, which have half widths (radii) at half the maximum intensity in the range 45-80 km. We compare the shape and width of lightning flashes in the images with simulated flashes produced by our 3D Monte Carlo light-scattering model.The model calculates Monte Carlo scattering of photons in a 3D opacity distribution. During each scattering event, light is partially absorbed. The new direction of the photon after scattering is chosen according to a Henyey-Greenstein phase function. An image from each direction is produced by accumulating photons emerging from the cloud in a small range (bins) of emission angles. The light source is modeled either as a point or a vertical line.A plane-parallel cloud layer does not always fit the data. In some cases the cloud over the light source appears to resemble cumulus clouds on Earth. Lightning is estimated to occur at least as deep as the bottom of the expected water cloud. For the six flashes studied, we find that the clouds above the lightning are optically thick (τ>5). Jovian flashes are more regular and circular than the largest terrestrial flashes observed from space. On Jupiter there is nothing equivalent to the 30-40-km horizontal flashes that are seen on Earth.  相似文献   

Lunisolar torque on the atmosphere and Earth's rotation     

C. Bizouard  S. Lambert 《Planetary and Space Science》2002,50(3):323-333

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书法景观的文化地理浅释   总被引：8，自引：2，他引：6  

吴慧平  司徒尚纪 《地理科学》2002,22(6):757-762

书法地理学作为一门新兴的文化地理学的分支,它的基本理论研究对象之一便是书法景观。从文化地理学的角度出发,探讨了书法景观的概念,书法景观的分类。指出其构成除了自然因素以外,还应包括人文景观中的可视性因素、可悟性因素和氛围。书法景观是自然景观人文景观的统一体。  相似文献   

Mapping of Ozone and Water in the Atmosphere of Mars near the 1997 Aphelion     

Robert E. NovakMichael J. Mumma  Michael A. DiSanti  Neil Dello Russo  Karen Magee-Sauer 《Icarus》2002,158(1):14-23

We present absolute abundances and latitudinal variations of ozone and water in the atmosphere of Mars during its late northern spring (L_s=67.3°) shortly before aphelion. Long-slit maps of the a¹Δ_g state of molecular oxygen (O₂) and HDO, an isotopic form of water, were acquired on UT January 21.6 1997 using a high-resolution infrared spectrometer (CSHELL) at the NASA Infrared Telescope Facility. O₂(a¹Δ_g) is produced by ozone photolysis, and the ensuing dayglow emission at 1.27 μm is used as a tracer for ozone. Retrieved vertical column densities for ozone above ∼20 km ranged between 1.5 and 2.8 μm-atm at mid- to low latitudes (30°S-60°N) and decreased outside that region. A significant decrease in ozone density is seen near 30°N (close to the subsolar latitude of 23.5°N). The rotational temperatures retrieved from O₂(a-X) emissions show a mean of 172±2.5 K, confirming that the sensed ozone lies in the middle atmosphere (∼24 km). The ν₁ fundamental band of HDO near 3.67 μm was used as a proxy for H₂O. The retrieved vertical column abundance of water varies from 3 precipitable microns (pr-μm) at ∼30°S to 24 pr-μm at ∼60°N. We compare these results with current photochemical models and with measurements obtained by other methods.  相似文献   

Microwave Remote Sensing of the Temperature and Distribution of Sulfur Compounds in the Lower Atmosphere of Venus     

Jon M. JenkinsMarc A. Kolodner  Bryan J. ButlerShady H. Suleiman  Paul G. Steffes 《Icarus》2002,158(2):312-328

A multi-wavelength radio frequency observation of Venus was performed on April 5, 1996, with the Very Large Array to investigate potential variations in the vertical and horizontal distribution of temperature and the sulfur compounds sulfur dioxide (SO₂) and sulfuric acid vapor (H₂SO₄(g)) in the atmosphere of the planet. Brightness temperature maps were produced which feature significantly darkened polar regions compared to the brighter low-latitude regions at both observed frequencies. This is the first time such polar features have been seen unambiguously in radio wavelength observations of Venus. The limb-darkening displayed in the maps helps to constrain the vertical profile of H₂SO₄(g), temperature, and to some degree SO₂. The maps were interpreted by applying a retrieval algorithm to produce vertical profiles of temperature and abundance of H₂SO₄(g) given an assumed sub-cloud abundance of SO₂. The results indicate a substantially higher abundance of H₂SO₄(g) at high latitudes (above 45°) than in the low-latitude regions. The retrieved temperature profiles are up to 25 K warmer than the profile obtained by the Pioneer Venus sounder probe at altitudes below 40 km (depending on location and assumed SO₂ abundance). For 150 ppm of SO₂, it is more consistent with the temperature profile obtained by Mariner 5, extrapolated to the surface via a dry adiabat. The profiles obtained for H₂SO₄(g) at high latitudes are consistent with those derived from the Magellan radio occultation experiments, peaking at around 8 ppm at an altitude of 46 km and decaying rapidly away from that altitude. At low latitudes, no significant H₂SO₄(g) is observed, regardless of the assumed SO₂ content. This is well below that measured by Mariner 10 (Lipa and Tyler 1979, Icarus39, 192-208), which peaked at ∼14 ppm near 47 km. Our results favor ≤100 ppm of SO₂ at low latitudes and ≤50 ppm in polar regions. The low-latitude value is statistically consistent with the results of Bézard et al. (1983, Geophs. Res. Lett.20, 1587-1590), who found that a sub-cloud SO₂ abundance of 130±40 ppm best matched their observations in the near-IR. The retrieved temperature profile and higher abundance of H₂SO₄(g) in polar regions are consistent with a strong equatorial-to-polar, cloud-level flow due to a Hadley cell in the atmosphere of Venus.  相似文献