Assessment of Dust Aerosol Optical Depth and Shortwave Radiative Forcing over the Northwest Pacific Ocean in Spring Based on Satellite Observations          下载免费PDF全文

CHEN Lin  SHI Guang-Yu  ZHONG Ling-Zhi  TAN Sai-Chun 《大气和海洋科学快报》2009,2(4):224-229

Dust aerosol optical depth （AOD） and its accompanying shortwave radiative forcing （RF） are usually simulated by numerical models. Here, by using 9 months of Moderate Resolution Imaging Spectroradiometer （MODIS） aerosol product data in combination with Clouds and the Earth＇s Radiant Energy System Single Scanner Footprint （CERES/SSF） data, dust AOD and its shortwave RF were estimated over the cloud-free northwest （NW） Pacific Ocean in the springs of 2004, 2005, and 2006. The results showed that in this region, the mean dust AOD and its shortwave RF were 0.10 and -5.51 W m^-2, respectively. In order to validate the dust AOD derived by MODIS, results from the Goddard Global Ozone Chemistry Aerosol Radiation and Transport （GOCART） model were also used here. The correlation coefficient between the monthly averaged dust AOD derived by MODIS measurements and the model simulation results was approximately 0.53. Since the estimates of the dust AOD and its shortwave RF obtained in this study are based mainly on satellite data, they offer a good reference for numerical models.  相似文献   

中国春季沙尘暴年代际变化和季节预测   总被引：2，自引：0，他引：2  

祝从文  徐康  张书萍  郭玲 《气象科技》2010,38(2):201-204

利用1954～2007年中国258个台站观测的月沙尘暴日数资料,北半球地表温度和美国NCAR/NCEP大气再分析资料,研究了中国春季沙尘暴日数年代际变化特征及其影响因子。研究发现:中国春季沙尘暴日数与贝加尔湖地表变暖存在显著的负相关,相关系数达到-0.8,该地区的地表温度变暖导致蒙古气旋活动和我国沙尘暴频率降低。利用该地区冬季对流层850 hPa温度与春季地表温度指数之间显著正相关关系,建立了冬季850 hPa温度指数预测中国春季沙尘暴频率的线性预报方程。通过22年回报检验发现,统计预报结果与多数台站观测的沙尘暴发生频率存在显著的正相关,最大相关系数达到+0.4。其中,近22年的预报场与观测之间空间相关系数平均达到+0.4以上,均方根误差在1～2之间,表明该统计预报模型具有一定的业务应用价值。  相似文献   

基于船载太阳光度计观测的黄海海面亚洲沙尘柱总量和干沉降通量个例研究   总被引：1，自引：0，他引：1       下载免费PDF全文

YANG Dong-Xu  LIU Yi  CHEN Wen-Zhong 《大气和海洋科学快报》2010,3(2):64-69

The total dust column and the dry deposition flux were calculated based on the optical properties that were measured by a shipboard sun photometer POM-01 MKⅡ in a cloud-free and nonfrontal dust condition on 24 April 2006. The total dust column was calculated by using an integration method of the particle size distribution; the mean value was 1.42±0.30 g m-2. A linear correlation between the total dust column and the aerosol optical depth (AOD) with a linear factor of 2.7 g m-2 over the Sahara was applied to calculate the total dust column in this study; the results were lower than these calculated by the integration method. A reasonable factor of 3.2 g m-2 was achieved by minimizing the standard deviation (SD) of the two methods. The two layers model, which includes the deposition processes of turbulent transfer, Brownian diffusion, impaction and gravitational settling over the sea’s surface, was used to calculate the dry deposition flux; the mean value was 5.05±2.49 μg m-2 s-1. A correlation among the total dust column, dry deposition flux, AOD, and effective radius was discussed. The correlation between the total dust column and the AOD was better than that between the total dust column and the effective radius; however, the correlation between the dry deposition flux and the effective radius was better than that between the dry deposition flux and the AOD.  相似文献   

The Northern Path of Asian Dust Transport from the Gobi Desert to North America   总被引：1，自引：0，他引：1       下载免费PDF全文

CHEN Ke-Yi 《大气和海洋科学快报》2010,3(3):155-159

The aerosol index (AI) of the Total Ozone Mapping Spectrometer (TOMS) satellite data (1979 2001) was analyzed to reveal the climatological long-distance path of dust transport from Asia to North America. The AI in the west coast of the United States is highly correlated with that in the Gobi desert. Additionally, from the TOMS satellite images, it can be seen that very strong plumes advect from Asia to the west coast of North America in typical dust storm cases. When applying the sourcereceptor relationship to detect the northern dust transport path between the Gobi source region and the west coast of the United States receptor region, it is evident that the dust plume can be transported northward beyond 60°N from its source region and that it takes 5 to 6 days to reach the west coast of the United States. The cross correlation technique shown in this work is a useful tool that can be applied in other regions to give useful insights into relationships between major dust sources and downwind receptor locations by using remotely sensed dust observations.  相似文献   

Impact of Saharan dust on PM10 concentration in the Mediterranean Tunisian coasts     

Karim Bouchlaghem  Blaise Nsom  Noureddine Latrache  Houda Haj Kacem 《Atmospheric Research》2009,92(4):531-539

This paper presents samples of Saharan dust outbreak affecting the Mediterranean Tunisian coasts and its impact on PM10 (Particles with an aerodynamic diameter below 10 µm) surface concentrations measured at seven monitoring stations during summer 2006. During the events, the daily PM10 levels at all stations exceeded EU and Tunisian air quality standard limits which are equal to 50 µg/m³. The maximum values ranged from 200 µg/m³ to 300 µg/m³ depending on the monitoring station. The impact is even more dramatic on PM10 hourly concentrations leading to maximum hourly peaks ranging from 400 µg/m³ to 850 µg/m³ again depending on the monitoring station (industrial or residential, traffic and commercial). Comparison between backward air masses trajectories reaching Tunisian coasts and satellite imageries vis-à-vis the PM10 hourly concentrations measured at the monitoring stations during 2006 evidenced the influence of the Saharan dust outbreaks on surface concentrations. The origin of the air masses is found to be from South-West direction under the influence of air masses from the Algerian Saharan desert.  相似文献   

A dynamical model of the sporadic meteoroid complex     

Paul Wiegert  Jeremie Vaubaillon 《Icarus》2009,201(1):295-310

Sporadic meteoroids are the most abundant yet least understood component of the Earth's meteoroid complex. This paper aims to build a physics-based model of this complex calibrated with five years of radar observations. The model of the sporadic meteoroid complex presented here includes the effects of the Sun and all eight planets, radiation forces and collisions. The model uses the observed meteor patrol radar strengths of the sporadic meteors to solve for the dust production rates of the populations of comets modeled, as well as the mass index. The model can explain some of the differences between the meteor velocity distributions seen by transverse versus radial scatter radars. The different ionization limits of the two techniques result in their looking at different populations with different velocity distributions. Radial scatter radars see primarily meteors from 55P/Tempel-Tuttle (or an orbitally similar lost comet), while transverse scatter radars are dominated by larger meteoroids from the Jupiter-family comets. In fact, our results suggest that the sporadic complex is better understood as originating from a small number of comets which transfer material to near-Earth space quite efficiently, rather than as a product of the cometary population as a whole. The model also sheds light on variations in the mass index reported by different radars, revealing it to be a result of their sampling different portions of the meteoroid population. In addition, we find that a mass index of s=2.34 as observed at Earth requires a shallower index (s=2.2) at the time of meteoroid production because of size-dependent processes in the evolution of meteoroids. The model also reveals the origin of the 55° radius ring seen centered on the Earth's apex (a result of high-inclination meteoroids undergoing Kozai oscillation) and the central condensations seen in the apex sources, as well as providing insight into the strength asymmetry of the helion and anti-helion sources.  相似文献   

Measurements of the Gegenschein brightness from the Solar Mass Ejection Imager (SMEI)     

Andrew Buffington  Mario M. Bisi  P. Paul Hick  Thomas A. Kuchar 《Icarus》2009,203(1):124-176

The Gegenschein is viewed by the Solar Mass Ejection Imager (SMEI), which has provided near-full-sky broadband visible-light photometric maps for over 5 years. These have an angular resolution of about 0.5° and differential photometric stability of about 1% throughout this time. When individual bright stars are removed from the maps and an empirical sidereal background subtracted, the residue is dominated by the zodiacal light. The unprecedented sky coverage and duration of these measurements enables a definitive characterization of the Gegenschein. This article describes the analysis method for these data, presents a movie with time of the Gegenschein brightness distribution, determines empirical formulae describing its average shape, and discusses its variation with time. These measurements unambiguously confirm previous reports that the Gegenschein surface-brightness distribution has a decided peak in the antisolar point, which rises above a broader background.  相似文献   

Evidence from IRAS for a very young, partially formed dust band     

Ashley J. Espy  Stanley F. Dermott  Sumita Jayaraman 《Planetary and Space Science》2009,57(2):235-242

The relative proportions of asteroidal and cometary materials in the zodiacal cloud is an ongoing debate. The determination of the asteroidal component is constrained through the study of the Solar System dust bands (the fine-structure component superimposed on the broad background cloud), since they have been confidently linked to specific, young, asteroid families in the main belt. The disruptions that produce these families also result in the injection of dust into the cloud and thus hold the key to determining at least a minimum value for the asteroidal contribution to the zodiacal cloud. There are currently known to be at least three dust band pairs, one at approximately 9.35° associated with the Veritas family and two central band pairs near the ecliptic, one of which is associated with the Karin subcluster of the Koronis family. Through careful co-adding of almost all the pole-to-pole intensity scans in the mid-infrared wavebands of the Infrared Astronomical Satellite (IRAS) data set, we find strong evidence for a partial Solar System dust band, that is, a very young dust band in the process of formation, at approximately 17° latitude. We think this is a confirmation of the M/N partial band pair first suggested by Sykes [1988. IRAS observations of extended zodiacal structures. Astrophys. J. 334, L55-L58]. The new dust band appears at some but not all ecliptic longitudes, as expected for a young, partially formed dust band. We present preliminary modeling of the new, partial dust band which allows us to put constraints on the age of the disruption event, the inclination and node of the parent body at the time of disruption, and the quantity of dust injected into the zodiacal cloud.  相似文献   

Shattering and coagulation of dust grains in interstellar turbulence     

Hiroyuki Hirashita  Huirong Yan 《Monthly notices of the Royal Astronomical Society》2009,394(2):1061-1074

We investigate shattering and coagulation of dust grains in turbulent interstellar medium (ISM). The typical velocity of dust grain as a function of grain size has been calculated for various ISM phases based on a theory of grain dynamics in compressible magnetohydrodynamic turbulence. In this paper, we develop a scheme of grain shattering and coagulation and apply it to turbulent ISM by using the grain velocities predicted by the above turbulence theory. Since large grains tend to acquire large velocity dispersions as shown by earlier studies, large grains tend to be shattered. Large shattering effects are indeed seen in warm ionized medium within a few Myr for grains with radius   a ≳ 10⁻⁶  cm. We also show that shattering in warm neutral medium can limit the largest grain size in ISM  ( a ∼ 2 × 10⁻⁵ cm)  . On the other hand, coagulation tends to modify small grains since it only occurs when the grain velocity is small enough. Coagulation significantly modifies the grain size distribution in dense clouds (DC), where a large fraction of the grains with   a < 10⁻⁶ cm  coagulate in 10 Myr. In fact, the correlation among   R_V   , the carbon bump strength and the ultraviolet slope in the observed Milky Way extinction curves can be explained by the coagulation in DC. It is possible that the grain size distribution in the Milky Way is determined by a combination of all the above effects of shattering and coagulation. Considering that shattering and coagulation in turbulence are effective if dust-to-gas ratio is typically more than ∼1/10 of the Galactic value, the regulation mechanism of grain size distribution should be different between metal-poor and metal-rich environments.  相似文献   

A refined model for spinning dust radiation     

Yacine Ali-Haïmoud  Christopher M. Hirata  Clive Dickinson 《Monthly notices of the Royal Astronomical Society》2009,395(2):1055-1078

We present a comprehensive treatment of the spectrum of electric dipole emission from spinning dust grains, updating the commonly used model of Draine & Lazarian. Grain angular velocity distributions are computed using the Fokker–Planck equation; we revisit the drift and diffusion coefficients for the major torques on the grain, including collisions, grain-plasma interactions and infrared emission. We use updated grain optical properties and size distributions. The theoretical formalism is implemented in the companion code, spdust , which is publicly available. The effect of some environmental and grain parameters on the emissivity is shown and analysed.  相似文献