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1.
The present study combined remote sensing with geographical information system (GIS) technology to interpret Landsat TM images from 1996 to 2000 and establish a land cover database for the Hexi Corridor of China’s Gansu Province. The areas of sand and dust emission and trends in their change were extracted by analyzing the database, with the following results: In 2000, the source area for sand and dust storms totaled nearly 170,000 km2, accounting for 75.1% of the study region. The emission area decreases from as much as 70,000 km2 in winter and spring to around 58,000 km2 in summer and autumn, accounting for 41.1 and 34.1% of the source area, respectively. During the 4 years of the study period, the emission area decreased by nearly 57 km2 in winter and spring (a 0.1% change); however, the vulnerability of the land surface to wind erosion increased in ca. 190 km2 and decreased in ca. 102 km2. Although the area of dust emission decreased from 1996 to 2000, the area vulnerable to wind erosion increased by ca. 87 km2, and the increased number of sand and dust storm days in the region between 2000 and 2003 appears to be correlated with this increase.  相似文献   

2.
The annual and seasonal dust emissions were calculated for eight types of desertified lands at 120 sites in the Heihe River Basin of northwestern China. The results showed that dust emission rates increased from the middle to the lower reaches of the river by a factor of up to 103. There two strongest areas of dust emission are the dried-up Gaxun Lake with a dust emission rate of 1.6 t ha−1 year−1, and the desertified grassland areas around the abandoned Heicheng City, with a dust emission rate of 0.6–0.7 t ha−1 year−1. The total annual dust emissions with their particle diameters less than 50, 30, and 10 μm were 1.71 × 106, 1.11 × 106, and 0.555 × 106 t, respectively. Dust emission rates showed striking seasonal variations, with the maximum value (45%) occurring in spring and the minimum value (13.5%) in summer. The mineral aerosol-size distributions were also measured and the results showed that the size distributions for dust and non-dust events were both trimodal, in contrast with the widely accepted view that primary particles such as aeolian dust are coarse, whereas particles less than 1 μm in diameter are mainly secondary particulate substances such as ammonium nitrate, ammonium sulfate, and organic matter.  相似文献   

3.
Our analysis of many years of infrared photometry of the unique object FG Sge indicates that the dust envelope formed around the supergiant in August 1992 is spherically symmetrical and contains compact, dense dust clouds. The emission from the spherically symmetrical dust envelope is consistent with the observed radiation from the star at 3.5–5 µm, and the presence of the dust clouds can explain the radiation observed at 1.25–2.2 µm. The mean integrated flux from the dust envelope in 1992–2001 was ～(1.0±0.2)×10?8 erg s?1cm?2. The variations of its optical depth in 1992–2001 were within 0.5–1.0. The maximum density of the dust envelope was recorded in the second half of 1993 and corresponded to mean optical depths as high as unity. Several times in the interval from 1992 to 2001, the dusty material of the envelope partially dissipated and was then replenished. For example, the optical depth of the dust cloud at λ=1.25 µm during the last brigthness minimum in the J band was τ1.25≈4.3, which is much higher than the optical depth of the dust envelope of FG Sge. During maxima of the J brightness, the mean spectral energy distribution at 0.36–5 µm can be represented as a combination of radiation from a G0 supergiant that is attenuated by a dust envelope with a mean optical depth of 0.65±0.15 and emission from the spherically symmetrical dust envelope itself, with the temperature of the graphite grains being 750±150 K. At minima of the J brightness, only radiation from the dust envelope is observed at 1.65–5 µm, with the radiation from the supergiant barely detectable at 1.25 µm. As a result, the integrated flux during J minima is almost half that during J maxima. The mean mass of the spherically symmetrical dust envelope of FG Sge in 1992–2001 was (3 ± 1) × 10?7M⊙. This envelope’s mass varied by nearly a factor of two during 1992–2001, in the range (2 – 4) × 10?7M⊙. In Autumn 1992, the mass-loss rate from the supergiant exceeded 2 × 10?7M⊙/yr. The average rate at which matter was injected into the envelope during 1993–2001 was 10?8M⊙/yr. The mean rate of dissipation of the dust envelope was about 1 × 10?8M⊙/yr. During 1992–2001, the supergiant lost about 8.7 × 10?7M⊙. The parameters of the dust envelope were relatively constant from 1999 until the middle of 2001.  相似文献   

4.
We describe the formation of carbon dust in binary systems with hot components as a result of the collisions of clouds in a two-phase stellar-wind model. Calculations are made for the well studied system WR 140. The collisions lead to the formation of composite clouds and shock waves, with the temperature at the shock front equal to about 3×108 K along both sides of the interface boundary. During isobaric deexcitation to (0.5–0.7)×104 K, the cloud density increases by a factor of several thousand; its thickness in the direction of the shock decreases by the same factor. After deexcitation, the hydrogen inside the composite cloud is in its atomic state, while the carbon remains ionized. The deexcitation is followed by expansion of the cloud, which moves away from both stars. During the first 106 s, its thickness remains relatively small, so that the expansion is one-dimensional. The radiation field inside the cloud decays, resulting in the recombination of the carbon. Further expansion of the cloud leads to adiabatic cooling, and the formation of dust particles becomes possible. After the dimensions of the cloud have become roughly the same in all directions, its expansion is isotropic, so that it becomes transparent within approximately 106 s, and the dust is heated to (1.0–1.4)×103 K, observed as an IR “lare.” The time required for the cloud to move from the exciting star and heat the dust is comparable to the observed delay in the increased IR emission relative to the time of periastron.  相似文献   

5.
Field experiments of aeolian dust accumulation on rock fragment substrata   总被引：3，自引：0，他引：3  
The effect of rock fragments and rock fragment cover on the accumulation of airborne dust was examined in a long-term field experiment in the Negev desert of Israel. Four parameters were studied: pebble eccentricity, pebble size, pebble flattening and cover density. The effect of these parameters on the accumulation of dust on the pebbles, on the accumulation of dust between and underneath the pebbles, and on total dust accumulation (pebbles+interpebble space) was measured separately. Accumulation on the pebbles increased as the pebbles became larger, less flattened and more elongated, and as cover density increased. Accumulation between and underneath the pebbles increased as the pebbles became smaller, more flattened and more elongated, and as cover density increased (although the accumulation area available became smaller). Total dust accumulation increased as the pebbles became smaller, more flattened and more elongated, and as cover density increased. Rock fragments act as a dust trap as dust accumulation on pebble-covered surfaces is several tens of times larger than dust accumulation on similar but pebble-free surfaces. However, less than 20% of the initially settled dust is protected from further erosion. In the Negev desert, dust erosion by wind is of the order of 10 times larger than dust erosion by water. The rate of long-term dust accumulation in the Negev is of the order of 15–30 g.m?2.yr?1. This is considerably lower than the rates proposed elsewhere in the literature, which are based upon over optimistic dust retainment percentages.  相似文献   

6.
A self-consistent model for the chemical-dynamical evolution of a region of ionized hydrogen around a massive young star and of the surrounding molecular gas is presented. The model includes all main chemical and physical processes, namely the photoionization of atomic hydrogen, photodissociation of molecular hydrogen and other molecules, and the evaporation of molecules from the mantles of dust particles. Heating and cooling processes are taken into account in the temperature calculations, including cooling in molecular and atomic lines. The hydrodynamical equations were solved using the Zeus2D hydrodynamical software package. This model is used to analyze the expansion of a region of ionized hydrogen around massive stars (effective temperature of 30 000 and 40 000 K) in a medium with various initial density distributions. The competition between evaporation from dust mantles and the photodissociation of molecules results in the formation of a transition layer between the hot HII region and cool quiescent medium, characterized by high abundances of molecules in the gas phase. The thickness of the transition layer is different for different molecules. Since there is a velocity gradient along the transition layer, and the maxima in the distributions of different molecules are at different distances from the star, observations of molecular emission lines should reveal distinction in shifts of lines of different molecules relative to the velocity of the quiescent gas. Such shifts have indeed been detected during molecular observations of the region of ionized hydrogen Sh2-235. For an initial gas density of 103 cm?3, the increase in the abundances of H2O and H2CO in the transition layer after desorption from dust occurs gradually rather than in a jump-like fashion; therefore, the concept of a “evaporation front” can be used only formally. In addition, the distances between the evaporation fronts for different molecules are significant. At higher initial gas densities (104 cm?3), sharp evaporation fronts are formed for the different molecules, which are close to each other and to the shock front. In this case, it is possible to speak of a single evaporation front for CO, H2O, and H2CO.  相似文献   

7.
Near-surface atmospheric dust in Changsha city of China was analyzed in terms of morphological and geochemical composition. Morphological and chemical composition of the dust particles were analyzed by environmental scanning electron microscopy coupled with an energy-dispersive X-ray analyzer. Results indicated that the atmospheric dusts were mainly composed of spherule, plate, irregularly shaped and agglomerate, which contains variable sizes and amounts of particles. The dust particles could be categorized into five groups based on their chemical characteristic: Al-, Si-, Ca-, C-rich particles and aggregate. These particles and aggregate could be directly related to nearby polluting activities, such as building construction, traffic emission and coal combustion. The X-ray diffraction results show that the main minerals for atmospheric dust are gypsum, quartz and calcite. Mica, halloysite, montmorillonite, hematite, brushite, zeolite, sepiolite, feldspar, alite, dickite, SiS2, Fe6(OH)2CO3, FeSO4, CdSO4, Pb(NO)2O3, Al2SO4(OH)4, As2O3SO3, (NH4)2SO4, NH4Cl, K(NH4)·Ca(SO4)2·H2O are also detected in samples. The identification of heavy metals shows that the concentrations of Cr (403.5?mg?kg?1), Cu (126?mg?kg?1), Zn (1541.5?mg?kg?1), Cd (2.5?mg?kg?1) and Pb (348?mg?kg?1) in the atmospheric dust are much higher compared to background value of soil. It indicates that the heavy metal (Cr, Cu, Zn, Cd and Pb) in the atmospheric dust is mainly due to human activities. The identification of main sources of atmospheric dust collected in typical areas can help to control the polluting sources in urban area.  相似文献   

8.
Emission of neutral atoms (K and Na) and molecules (H2O and KOH) observed during fracture of K-feldspar have been accounted for by two independent mechanisms. H2O and KOH emissions are attributed to the venting of fluid-filled inclusions, while emission of atomic K is due to surface effects accompanying cleavage of crystalline feldspar. The intensity of emitted potassium, at least 6 × 1014 atoms/cm2 of surface area, is sufficient to affect K activities in solution during microbrecciation in the presence of rock-dominated fluids.  相似文献   

9.
We have calculated a model for the dust envelope of the protoplanetary nebula IRAS 18062+2410 using observations from the ultraviolet to the far infrared. We assume that the envelope is spherically symmetrical and consists of identical silicate grains with a radius of 0.10 micron, and with the number density of the grains inversely proportional to the square of the distance. The optical depth of the envelope, whose inner boundary is 1.40×10?3 pc from the center of the star, is 0.050 at 10 microns. At the inner envelope boundary, the temperature of the dust grains is 410 K and their density is 2.7×10?7 cm?3. Using calculations of stellar evolution at the stage following the exit from the asymptotic giant branch, we estimate the dust envelope’s expansion velocity to be 12 km/s. The mass-loss rate of the star preceding the ejection of the envelope was about 4.5×10?6 M ⊙/yr. The observed excess of far-IR flux is not associated with the continuum radiation of the nebula, and may provide evidence for the presence of dust ejected by the star in earlier stages of its evolution.  相似文献   

10.
A long dust history established using geological archives from dust provenance areas is necessary to understand the role of atmospheric dust in the global climate system better. Core sediments from a closed-basin groundwater-recharged lake in arid Central Asia were investigated using a multi-proxy approach (e.g. 14C AMS dating, pollen, and grain size) to trace the dust history since ~ 15 cal ka BP. Pollen analysis showed that before 7.9 cal ka BP, the vegetation was of desert type. After 7.9 cal ka BP, vegetation density increased, probably due to slightly increased moisture. The Chenopodiaceae-dominated desert expanded rapidly at 4.2–3.8 cal ka BP. Grain-size analysis was conducted for samples of lake deposits, modern aeolian dust, and dust trapped in snow, and the data showed that there was strong aeolian dust deposition at 11.8–11.1, 10.6–8, 6.1–4.9, and after 3.3 cal ka BP. This timing corresponds well with periods of increased terrestrial dust fluxes recorded by Greenland ice cores. Our study may document changes in the location and intensity of the Siberia High. These changes may play a more important role in the history of dust emission in arid Central Asia than previously thought.  相似文献   

11.
Beryllium isotope concentrations were determined in monthly rainfall collections at three sites across New Zealand (36 to 45° S), from October 1996 to November 1998. At the northern sites of Leigh (near Auckland) and Gracefield (near Wellington), 7Be and 10Be concentrations are relatively constant at 1.2 to 1.4 × 107 atoms kg−1 rain and 2.1 to 2.6 × 107 atoms kg−1 rain, respectively. These concentrations correspond to annual flux rates of ∼15 and ∼27 × 109 atoms m−2 y−1, respectively. At the southern site of Dunedin, concentrations are similar to those at the northern sites, but flux rates are significantly lower at ∼ 9 and ∼19 × 109 atoms m−2 y−1, respectively, because of lower average rainfall east of the Southern Alps mountain range. These results are broadly similar to those reported by Brown et al. (1989) and Knies et al. (1994) for rain from midlatitude sites in the USA sampled from 1986 to 1994. Mean 7Be/10Be ratios for New Zealand (0.47 to 0.61) are, however, significantly lower than for the USA (0.69 to 0.78), due in part to the addition of 10Be from re-suspended dust. Subtraction of the dust component increases the New Zealand 7Be/10Be ratios to 0.70 (Leigh), 0.65 (Gracefield) and 0.50 (Dunedin). The adjusted results provide evidence for transfer of older stratospheric air to the troposphere in late-spring-summer, an effect which is strongest in the north. The overall reduction of 7Be/10Be from north to south implies an increase in residence time from ∼ 80 to ∼100 d for Be isotopes in the atmosphere above New Zealand.  相似文献   

12.
The spatial and temporal variability of Hg emissions from urban paved surfaces was assessed through repeated measurements under varying environmental conditions at six sample sites in Toronto, Ontario, Canada. The results show significant spatial variability of the Hg emissions with median values ranging from below detection limit to 5.2 ng/m2/h. Two of the sites consistently had higher Hg emissions (on several occasions >20 ng/m2/h) than the other 4, which were equivalently low (maximum emission: 2.1 ng/m2/h). A surrogate measure of the pavement Hg concentrations was obtained during each day of sampling through the collection of street dust. The median street dust concentration also showed significant spatial variability (ranging from 9.6 to 44.5 ng/g). Regression analysis showed that the spatial variability of the Hg emissions was significantly related to the street dust concentrations. Controlled experiments using Hg amended street dust confirmed the relationship between Hg surface concentration and emission magnitude. Within a given sample site, Hg emissions varied temporally and multiple regression analysis showed that within-site variability was significantly influenced by changes in solar radiation with only a minor effect from surface temperature. Controlled experiments using shade cloths confirmed that solar radiation can have a large influence on the magnitude of Hg emissions within a given site. The emissions measured in Toronto were contextualized through comparison sampling in Austin, Texas. The Hg emissions measured in Austin were within the range detected in Toronto and also showed significant correlation with Hg street dust concentrations between sites. To provide a holistic assessment of Hg emissions from urban environments, samples were also collected from other common urban surfaces (soil, roofs, and windows). Soils consistently had higher emissions than all the other surfaces (7.3 ng/m2/h, n = 39).  相似文献   

13.
Helium has been proposed as a pathfinder in exploration for uranium deposits, hydrocarbons and geothermal energy sources, as an indicator of faults and fissures and as a possible tool for earthquake prediction. The rationale is that during the decay of 238U to 206 Pb, eight 4He atoms are produced via the intermediary of alpha particle emission. Similarly, six 4He atoms are produced by the decay of 232Th to 208Pb. Some of the common isotopes of the rare earths Ce, Nd and Sm are also alpha emitters, but they are unlikely to give rise to detectable helium anomalies.  相似文献   

14.
2006年3月11日南京“泥雨”降尘特征及其粉尘来源   总被引：2，自引：0，他引：2       下载免费PDF全文
对2006年春季南京地区一次“泥雨”形式的湿降尘特征进行了系统分析,并在此基础上对泥雨粉尘来源及泥雨降尘形成机制进行了探讨。结果表明：  1)本次泥雨降尘通量为3.77g/m2,在南京全境的降尘总量达到2.49×104t;   2)泥雨粉尘的质量磁化率值为174×10-8m3/kg,略高于黄土磁化率值; 3)泥雨粉尘中<16μm的细粒组分占绝对优势(含量为91.91％),平均粒径6.05μm,众数粒径7.68μm;   粒度参数及分布曲线显示泥雨粉尘具有比黄土和现代干降尘更好的分选性和更对称的峰态;   4)XRD和SEM分析表明,泥雨粉尘以絮状矿物颗粒为主,其中粘土矿物含量最高,占57.7％,其他矿物有石英(15.5％),钠长石(12.0％)和微量的白云石(1.0％);   5)泥雨粉尘的常量元素组成与黄土、现代干降尘以及上陆壳(UCC)大体相似,显示其主要为地壳源;   而微量元素中Zn,Co,Ni,Ba,Cr,V,Cu,Zr,Cd和Pb等重金属元素含量较黄土及UCC偏高,其中Zn,Cu,Cd和Pb等含量显著偏高,显示了地壳源之外的人为污染源的影响;   相比本地的下蜀黄土,南京泥雨粉尘样品的REE组成特征与北方黄土之间的相似程度更高,显示了更为密切的亲缘关系;   6)根据泥雨降尘的特征,结合天气活动过程,可以判定此次南京泥雨降尘并非本地扬尘所致,而主要来源于北方尘暴活动所产生的细粒粉尘;   寒潮冷锋的南侵提供了长距离输送动力,而长江下游海洋性暖湿气流对细粒粉尘的清除过程则最终导致了泥雨的形成;   南京春季泥雨降尘事件实质上是长江下游地区对西北内陆干旱区沙尘暴活动的一种区域响应。  相似文献   

15.
玉龙雪山地区大气降水中粉尘颗粒物特征研究   总被引：4，自引：1，他引：3  
以在玉龙雪山地区采集的大气降水样品为主要研究载体,分析了大气降水中粉尘颗粒物随时间的变化特征和影响大气降水中粉尘含量的潜在因素. 结果表明：大气降水中颗粒物浓度和典型粉尘特征化学离子含量的变化具有很好的一致性,且季风期末大气降水中的微粒含量显著升高,显示了明显的季节性变化特征. 丽江市和甘海子盆地大气降水中粉尘化学离子含量(SO42-,Mg2+,Ca2+,K+,NH4+,NO3-,粉尘浓度)之间具有较好的相关性,反映了这些离子共同的来源. 降水中pH值和电导率的变化很大程度上受到粉尘活动的影响,海盐气溶胶粒子对玉龙雪山地区大气降水中典型粉尘微粒(除Cl-和部分Na+之外)的沉降没有贡献. 此外,降水化学和微粒分析表明,丽江市区的大气环境不排除人为活动的影响.  相似文献   

16.
The present work is an attempt to investigate pollution effect on an ornamental tree species Thevetia peruviana (Pers.) K. Schum. The study was conducted in various green spaces of institutional, industrial, residential and near traffic site representing as different status of air pollution concentration depending on land-use type. The resistance index calculated for selected species had mean value of 14.57 ± 0.41 observed at study sites. The dust deposition was found in range of 5.14–7.74 mg cm?2 on foliar surface of 12 cm2. The examination of leaf structure with scanning electron microscope showed presence of airborne dust particles in coarse and fine sizes with higher deposition found in industrial and residential sites. The epicuticular wax layer on upper surface of foliar was found eroded at industrial and traffic regions. The equivalent diameter of particles was observed to range from 0.45 to 12.71 µm in Poisson distributional pattern. The density of number concentration of dust particles was observed 1411 and 3703 in institutional and industrial area deposited on 0.22 mm2 of foliar surface. The elemental distribution on leaves of Thevetia peruviana has revealed a mixture of carbonaceous and soil matrix elements such as C, O, Al, Na, Si, K and Mg observed in proportion of X-rays counts per second. The whole experiment gave a positive indication for plant species as a tolerant bio-indicator of air pollutants in Delhi. The diverse flora present in city provides an opportunity for reducing harmful concentration of PM10 and PM2.5 and improving quality of air for human health.  相似文献   

17.
Total suspended particulate samples (TSP) were collected and concentrations measured during seventeen months in the vicinity of a ceramic industrial area. A method of fractionating was applied to the samples in order to obtain two fractions corresponding to mineral particulate coming from dust emissions (Upper-F fraction) and to amorphous matter (carbon plus small amounts of S, Ca, Fe, etc) coming mainly from traffic and other combustion processes. Also for TSP samples several element concentrations were measured following two previous treatments: extraction of elements mainly associated with the soluble fraction of the samples (B, Fe, P, As, NO2–, NH4+, Cl–, F) and acid digestion for trace metals and elements mainly associated with the non-soluble fractions of the samples (Fe, As, Cd, Ni, Pb, Zn Ca). Seasonal differences and the influence of meteorological parameters (temperature, relative humidity, pressure and wind conditions) on the air pollution levels, particles as well as ions, were studied.Results show different seasonal and weekly evolution for mineral and amorphous carbonaceous particles because of the different origins in dust emissions or combustion processes respectively, and the different physical properties such as size grain. Of the ions analyzed Fe, Ca and Zn were clearly associated to mineral phases and consequently related to dust emissions, and NO2–, NH4+, P, Cl– were related to amorphous matter coming from combustion. Ni and Cd show lower levels than those reported as guideline values and the source is mainly related to the enrichment of these elements in clay materials. B and As content result in elevated concentrations, with the tendency to increase during cold months. The emission of these elements was associated with vaporization or volatilization during high temperature ceramic processes. The original gaseous state is influenced by temperature. In the winter the content for B and As is higher due to enhanced condensation of gas-phase boron onto particles, while in the summer the increase of air temperature results in elevated evaporation.  相似文献   

18.
A model for the dust envelope of the protoplanetary nebula LSIV-12°111 is computed using measured fluxes of the object from the UV to the far-IR. It is assumed that the spherically symmetrical envelope is comprised of silicate particles with a standard MRN size distribution, whose number density varies inversely proportional to the square of the distance. The optical depth of the envelope, whose inner boundary is 5.6×1016 cm from the central star, is 0.072 at 0.55 µm. The temperature of the dust grains at the inner boundary of the envelope is 124 K. The estimated distance to LSIV-12°111 is 3.8 kpc. The current mass-loss rate of the object derived from a self-consistent solution for the radiative transport and motion of the dust in the envelope is 1.0×10?5M⊙/yr.  相似文献   

19.
Observations of various types of objects in the northern sky were obtained at 44 GHz in the 70-61 A + methanol line on the 20-m Onsala radio telescope (Sweden), in order to search for Class I methanol maser emission in the interstellar medium: regions of formation of high-mass stars, dust rings around HII regions, and protostellar candidates associated with powerful molecular outflows and Galactic HII regions. Seven new Class Imethanolmasers have been discovered toward regions of formation of highmass stars, and the existence of two previously observed masers confirmed. The following conclusions are drawn: (1) neither the association of a bipolar outflow manifest in the wings of CO lines with a highmass protostellar object (HMPO) nor the presence of thermal emission in lines of complex molecules are sufficient conditions for the detection of Class I methanol emission; no association with HMPOs radiating at 44 GHz was found for EGOs (a new class of object tracing bipolar outflows); (2) the existence of H2O masers and Class II methanol masers in the region of aHMPOenhances the probability of detecting Class I methanol emission toward the HMPO; Class II methanol masers with stronger line fluxes are associated with Class I methanol masers.  相似文献   

20.
The characteristics of sand and dust movement over different sandy grasslands in China’s Otindag Sandy Land were explored based on field observations and laboratory analyses. Threshold wind speeds (the speed required to initiate sand movement) at a height of 2 m above the ground were estimated in the field for different surface types. Threshold wind speed above shifting dunes in the study area is about 4.6 m s−1 at this height. This value was smaller than values observed above other surfaces, resulting in a greater risk of blowing sand above these dunes. Differences in sand transport rates (STR) as a function of the severity of desertification resulted primarily from differences in surface vegetation cover and secondarily from the soil’s grain-size distribution. STR increased exponentially with increasing near-bed wind velocity. Under the same wind conditions, STR increased with increasing severity of desertification: from 0.08 g cm−2 min−1 above semi-fixed dunes to 8 g cm−2 min−1 above semi-shifting dunes and 25 g cm−2 min−1 above shifting dunes. Vegetation’s affect on STR was clearly large. Different components of sand and dust were trapped over different lands: mostly sand grains but little dust were trapped above shifting dunes, but much dust was collected over semi-shifting and semi-fixed dunes. Human disturbance is likely to produce dust even from fixed dunes as a result of trampling by animals and vehicle travel. In addition, spring rainfall decreased the risk of sand and dust movement by accelerating germination of plants and the formation of a soil crust.  相似文献   

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