中蒙地区沙尘暴研究的若干进展   总被引：45，自引：1，他引：44       下载免费PDF全文

钱正安  蔡英  刘景涛  柳中明  李栋梁  宋敏红 《地球物理学报》2006,49(1):83-92

本文首先回顾了近20多年来我国沙尘暴研究的3个主要阶段,然后从沙尘观测、沙尘暴气候学、沙尘暴爆发和沙尘传输的环流型、沙尘暴活动的年代际变化和原因、以及待深入研究的问题等5方面简要评述了它的研究进展和问题. 指出中蒙沙尘主要来源于中国西北及蒙古国南部和西北部地区;随沙尘天气强度逐渐加强（即从背景大气到浮尘、扬沙、沙尘暴、强及特强沙尘暴）,它们的地面沙尘浓度约按3倍的比率依次递增;揭示了我国北方及蒙古国南部的七大沙尘暴多发区,沙尘暴主要出现在春季午后至傍晚间丰富的沙源,强风和不稳定的大气层结是形成沙尘暴的3个主要因子;中蒙地区沙尘暴爆发的环流主要有低压冷锋型和低压、冷锋加中尺度系统的强对流型两类,前者占绝大多数,后者是极少数,但为沙尘暴爆发短期预报的难点,沙尘的传输主要决定于低空环流型;近50年来中蒙地区的沙尘暴活动呈波动变化,而且中蒙中、东及西区三区系的变化不完全相同. 它们与北方风沙区生态环境恶化,特别是蒙古及日本海附近气旋频数的年代际变化有关;防御沙尘暴重点要抓上述七大多发区生态环境的治理及沙尘暴预警系统的建立,治理措施要因地制宜;要加强沙尘暴爆发和沙尘输送的数值预报和模拟研究.  相似文献   

一次蒙古气旋型强沙尘暴的数值模拟试验   总被引：4，自引：3，他引：1  

姜学恭  赵琳娜 《高原气象》2006,25(4):672-679

利用沙尘数值预报模式对一次典型的蒙古气旋沙尘暴过程进行了数值模拟试验,结果表明:模式对沙尘区范围、强度及蒙古气旋不同发展阶段沙尘暴的强度、位置和演变进行了较成功的模拟。这次过程沙尘主要源于蒙古国南部及我国内蒙古中、西部荒漠化地区,沙尘以细中粉沙为主(d≤22μm)。模式模拟的沙尘暴日变化强于实况,其原因是模式没有考虑沙尘气溶胶辐射反馈机制。沙尘气溶胶的辐射强迫将削弱大气层结的日变化,从而有利于沙尘暴强度的维持。  相似文献   

中国北方沙尘灾害影响因子分析   总被引：8，自引：0，他引：8  

范一大  史培军  周涛  李仪 《地球科学进展》2007,22(4):350-356

利用中国北方1951—2000年188个沙尘暴代表站的气象观测数据和1983—2000年EROS数据中心NDVI数据,对我国北方沙尘灾害的影响因子进行了分析。主要结论有：①在影响沙尘暴发生、发展、演化的自然因子中,植被覆盖度、降水、大风日数和温度起关键作用,夏季植被覆盖度对来年春季沙尘暴发生频次影响较大,降水和温度主要表现在对地表植被覆盖等与沙尘暴有关的地表参数的影响;②大风日数和温度是沙尘暴形成的动力因子,植被覆盖度和降水是阻力因子。沙尘暴日数和持续时间的变化,主要取决于动力因子与阻力因子的综合作用;③遏制沙尘灾害的治本办法,不在于治理沙尘暴本身,而在于消除产生土地退化、生态安全下降的社会原因,处理好发展与生态环境建设的关系。  相似文献   

Direct Monte Carlo and multifluid modeling of the circumnuclear dust coma: Spherical grain dynamics revisited     

J.-F. Crifo  G.A. Loukianov  V.V. Zakharov 《Icarus》2005,176(1):192-219

This paper describes the first computations of dust distributions in the vicinity of an active cometary nucleus, using a multidimensional Direct Simulation Monte Carlo Method (DSMC). The physical model is simplistic: spherical grains of a broad range of sizes are liberated by H₂O sublimation from a selection of nonrotating sunlit spherical nuclei, and submitted to the nucleus gravity, the gas drag, and the solar radiation pressure. The results are compared to those obtained by the previously described Dust Multi-Fluid Method (DMF) and demonstrate an excellent agreement in the regions where the DMF is usable. Most importantly, the DSMC allows the discovery of hitherto unsuspected dust coma properties in those cases which cannot be treated by the DMF. This leads to a thorough reconsideration of the properties of the near-nucleus dust dynamics. In particular, the results show that (1) none of the three forces considered here can be neglected a priori, in particular not the radiation pressure; (2) hitherto unsuspected new families of grain trajectories exist, for instance trajectories leading from the nightside surface to the dayside coma; (3) a wealth of balistic-like trajectories leading from one point of the surface to another point exist; on the dayside, such trajectories lead to the formation of “mini-volcanoes.” The present model and results are discussed carefully. It is shown that (1) the neglected forces (inertia associated with a nucleus rotation, solar tidal force) are, in general, not negligible everywhere, and (2) when allowing for these additional forces, a time-dependent model will, in general, have to be used. The future steps of development of the model are outlined.  相似文献   

Modelling dust distributions in the atmospheric boundary layer on Mars     

Peter A. Taylor  P-Y. Li  Diane V. Michelangeli  Jagruti Pathak  Wensong Weng 《Boundary-Layer Meteorology》2007,125(2):305-328

A time and height dependent eddy diffusion model is used to investigate possible scenarios for the size distribution of dust in the lower atmosphere of Mars. The dust is assumed to either have been advected from a distant source or to have originated locally. In the former case, the atmosphere is assumed to initially contain dust particles with sizes following a modified gamma distribution. Larger particles are deposited relatively rapidly while small particles are well mixed up to the maximum height of the afternoon boundary layer and are deposited more slowly. In other cases, a parameterization of the dust source at the surface is proposed. Model results show that smaller particles are rapidly mixed within the Martian boundary layer, while larger particles (r > 10 μm) are concentrated near the ground with a stronger diurnal cycle. In all simulations we assume that the initial concentration or surface source depend on a modified gamma function distribution. For small particles (cross- sectional area weighted mean radius, r_eff = 1.6 μm) distributions retain essentially the same form, though with variations in the mean and variance of the area-weighted radius, and the gamma function can be used to represent the particle size distribution reasonably well at most heights within the boundary layer. In the case of a surface source of larger particles (mean radius 50 μm) the modified gamma function does not fit the resulting particle size distribution. All results are normalised by a scaling factor that can be adjusted to correspond to an optical depth for assumed particle optical scattering properties.  相似文献   

地形对沙尘暴的影响及敏感试验研究   总被引：2，自引：3，他引：2  

沈建国  姜学恭  孙照渤 《高原气象》2007,26(5):1013-1022

在初步探讨地形影响沙尘扬升、传输、沉降等动力过程可能机制的基础上,利用沙尘数值预报模式对一次强沙尘暴过程进行了模拟研究,结果表明:沙尘暴形成阶段沙尘主要来源于阿尔泰—萨彦岭及以东地区,这部分沙尘主要向东扩展,该区域地形对其强度具有重要影响;内蒙古中西部、甘肃、宁夏等地的起沙主要在沙尘暴持续阶段产生影响,之后主要向南输送,青藏高原东侧地形绕流对其强度具有影响。地形影响可以使沙尘的扩展分为两种不同的方式,当上下游地形落差较小时形成整体推进式传输,此时沙尘位于对流层低层,没有上下沙尘层的分离;当上下游地形落差较大时形成分离式传输,沙尘位于对流层中层且在传输过程中沉降很弱,同时与地面附近的沙尘层分离。源于蒙古国、内蒙古等地的沙尘往往产生整体推进式传输;而产生于青藏高原的沙尘常形成分离式传输。  相似文献   

内蒙古“4．23”沙尘暴天气的环流背景及成因     

高玲  吕娜  任楠  拓砚军 《山西气象》2011,(2):4-8

利用常规观测资料和MICAPS提供的相关资料,对2009年4月23日－24日在内蒙古中西部地区发生的大范围大风、沙尘暴天气的高、低空环流形势、物理量场、卫星云图及数值预报场进行了分析。结果表明：a）本次沙尘暴的主要影响系统是贝加尔湖高空低涡引导冷空气南下在蒙古形成密集的高空锋区;b）地面蒙古气旋的暖性性质为沙尘暴的爆发提供了有利的热力条件;c）强烈的上升与下沉运动为大风、沙尘天气的发生提供了动力条件;d）螺旋状逗点云系的发展为此次大风、沙尘暴天气的形成提供了有利条件;e）沙尘暴发生前期上游地区干暖的气候条件及下垫面增厚的于土层及沙区,对沙尘暴的发生提供最基本的环境条件。  相似文献   

２种统计方法对气象要素均一性的影响          下载免费PDF全文

李亚丽  妙娟利 《陕西气象》2011,(3):29-32

在天气现象观测中,轻雾、霾、浮尘是较易混淆的天气现象,准确的判断和记录这些现象,需要从形成条件、天气背景、垂直能见度、相对湿度等方面进行分析,综合判断,本文对此作了一些分析和探讨。  相似文献   

The influence of the brightness of the asteroidal dust bands on the gegenschein     

Tadashi Mukai  Masanori Fujino  Ryosuke Nakamura  Fumihiko Usui 《Icarus》2003,162(2):337-343

The position and shape of the Gegenschein’s maximum brightness provide information on the structure of the interplanetary dust cloud. We show that the asteroidal dust bands, extended near the anti-solar point, play an important role in determining both the position of the maximum brightness and the shape of the Gegenschein. After removing the asteroidal dust bands from an observation of the Gegenschein on November 2, 1997, it was found that the maximum brightness point shifted −0.4° in ecliptic latitude, i.e., to the south of the ecliptic plane, at an ecliptic longitude of 180°, in contrast to a latitude value of +0.1° when the dust bands were included. Furthermore, the part of the Gegenschein to the south of the ecliptic plane was brighter than the northern part at the time of observation. Referring to the cloud model of T. Kelsall et al. (1998, Astrophy. J. 508, 44-73), it can be estimated that the ascending node of the symmetry plane of the dust cloud is 57°^−3°_+7° when its inclination is 2.03° ? 0.50°.  相似文献   

A dust cloud around Pluto and Charon     

K.-U. Thiessenhusen  A.V. Krivov  H. KrügerE. Grün 《Planetary and Space Science》2002,50(1):79-87

We suggest that Pluto and Charon are immersed in a tenuous dust cloud. The cloud consists of ejecta from Pluto and—especially—Charon, released from their surfaces by impacts of micrometeoroids originating from Edgeworth-Kuiper belt objects. The motion of the ejected grains is dominated by the gravity of Pluto and Charon, which determines a pear-shape of the densest part of the cloud. While the production rates of escaping particles from both sides are comparable, the lifetimes of the Charon particles inside the Hill sphere of Pluto-Charon with respect to the Sun are much longer than of the Pluto ejecta, so that the cloud is composed predominantly of Charon grains. The dust cloud is dense enough to be detected with an in situ dust detector onboard a future space mission to Pluto. The cloud's maximum optical depth of τ≈3×10⁻¹¹ is, however, too low to allow remote sensing observations.  相似文献