干旱区一次春季沙尘过程的大气气溶胶垂直分布结构及其特征

采用微脉冲激光雷达(Micro-Pulse Lidar,MPL)对干旱荒漠代表站张掖站上空一次春季沙尘暴过程的边界层和自由大气的气溶胶分布和大气环境进行了观测。结果表明,气溶胶的垂直廓线可分为高、中、低3层,高层气溶胶出现在5～9km,主要是通过上风方向的高海拔区域或低层气溶胶通过对流等过程突破边界层顶进入自由大气输送而来,其分布高度在一天中随着时间的推移逐渐降低;中层气溶胶位于2.5～4.5km,其消光特性随高度的增加没有明显的变化,具有垂直混合现象;低层气溶胶在2.5km以下,其消光特性随着高度增加反而降低;中、低层气溶胶主要来源于外部源区或当地沙尘源区和沙壤土起沙。气溶胶垂直分布表现出3种形式:在大气稳定条件下,气溶胶随高度增加呈单峰型减小趋势;不稳定条件下随高度增加指数型降低;混合层中随高度增加而保持稳定。由于受边界层日变化的影响,气溶胶分布的上界出现单峰型日变化特征,具体表现为下午较高,早晨较低。     

NOAA卫星沙尘暴光谱特征分析及信息提取研究

通过对2000—2002年多次沙尘暴过程NOAA卫星AVHRR资料的分析,研究了沙尘、云、沙漠、戈壁、积雪、裸地、植被等不同目标物的光谱特性,发现沙尘暴在AVHRR-2中各通道均有不同程度的反映。1,2通道中沙尘的反射率较高(介于云和沙漠之间);4,5通道的亮温低于晴空地表高于云;在3通道中沙尘表现的很独特,其亮度温度为所有研究目标物中最高的,表明通道3包含较多的沙尘信息,AVHRR-3取代AVHRR-2后对监测沙尘有不利影响。在此基础上提出定量提取沙尘信息的两种沙尘判识指数,并利用沙尘判识指数成功地提取多次沙尘暴过程的沙尘信息。结果表明：利用多通道组合沙尘判识指数能够对沙尘信息进行有效提取。     

Correlation between rainfall and dust occurrence at mildura,Australia: The difference between local and source area rainfalls

In studies of temporal variation in dust activity, rainfall recorded at the same location as the dust events (local rainfall) has commonly been used as a climatic control variable. The main objectives of this note are to test the validity of using local rainfall and to determine the improvement in the relationship between rainfall and dust activity that could be achieved by using regional rainfall in the dust source area. For the period 1960-1989 at Mildura, Australia, the likely dust source area was identified by analysing wind direction during dust events. It was found that a marked improvement in the correlation between dust activity and antecedent rainfall can be achieved by using the regional source area rainfall rather than local rainfall. The improved correlation suggests that widespread drought is more important than local below-average rainfall in intensifying dust activity.     

Follow-up observations of β-pic-like stars

Following the discovery, by IRAS, of the dust disc around Vega and three other main sequence stars, searches have been made for other candidates. The-Pic-like candidates have 12µm excesses and 100µm fluxes (unlike the Vega-like candidates), so they can be further investigated using ground-based techniques. Data are presented here, comprising 10µm spectroscopy and sub-mm observations, for several candidates from the Walker & Wolstencroft list, showing that the stars have silicate dust, and optically thick dust discs even at 1300µm.     

Quasiintegrals of the photogravitational eccentric restricted three-body problem with Poynting–Robertson drag

A restricted three-body problem for a dust particle, in presence of a spherical cometary nucleus in an eccentric (elliptic, parabolic or hyperbolic) orbit about the Sun, is considered. The force of radiation pressure and the Poynting– Robertson effect are taken into account. The differential equations of the particle’s non-inertial spatial motion are investigated both analytically and numerically. With the help of a complex representation, a new single equation of the motion is obtained. Conversion of the equations of motion system into a single equation allows the derivation of simple expressions similar to the integral of energy and integrals of areas. The derived expressions are named quasiintegrals. Relative values of terms of the energy quasiintegral for a smallest, largest, and a mean comet are calculated. We have found that in a number of cases the quasiintegrals are related to the regular integrals of motion, and discuss how the quasiintegrals may be applied to find some significant constraints on the motion of a body of infinitesimal mass.     

Charging and motion of dust grains near the terminator of the moon

We discuss the formation of strong local electric fields near minicraters or hills in the vicinity of the terminator. Electrons, having large thermal velocity compared to the solar wind speed can easily penetrate into the shadowed part of a minicrater. At the same time only protons with velocities much higher than their thermal speed can reach such regions. This results in the formation of a strong local negative potential whose magnitude depends on the steepness of the shadowed slope of the minicrater. The extremely small conductivity of the lunar regolith at the shadowed side of the crater prevents any significant electric discharge and thus supports the formation of a strong potential difference at scales much smaller than the Debye radius. Our estimates show that the created local electric fields are sufficiently strong enough to elevate dust grains with the sizes of the order of above the surface. The suggested mechanism is efficient only after sunset rather close to the terminator. Far away from the terminator at the dark side the fluxes of charged particles hitting the surface are so small that the process of dust elevation becomes too weak.     

Galileo in-situ dust measurements in Jupiter’s gossamer rings

Galileo was the first artificial satellite to orbit Jupiter. During its late orbital mission the spacecraft made two passages through the giant planet’s gossamer ring system. The impact-ionization dust detector on board successfully recorded dust impacts during both ring passages and provided the first in-situ measurements from a dusty planetary ring. During the first passage—on 5 November 2002 while Galileo was approaching Jupiter—dust measurements were collected until a spacecraft anomaly at 2.33R_J (Jupiter radii) just 16 min after a close flyby of Amalthea put the spacecraft into a safing mode. The second ring passage on 21 September 2003 provided ring dust measurements down to about 2.5R_J and the Galileo spacecraft was destroyed shortly thereafter in a planned impact with Jupiter. In all, a few thousand dust impacts were counted with the instrument accumulators during both ring passages, but only a total of 110 complete data sets of dust impacts were transmitted to Earth. Detected particle sizes range from about 0.2 to 5 μm, extending the known size distribution by an order of magnitude towards smaller particles than previously derived from optical imaging [Showalter, M.R., de Pater, I., Verbanac, G., Hamilton, D.P., Burns, J.A., 2008. Icarus 195, 361-377; de Pater, I., Showalter, M.R., Macintosh, B., 2008. Icarus 195, 348-360]. The grain size distribution increases towards smaller particles and shows an excess of these tiny motes in the Amalthea gossamer ring compared to the Thebe ring. The size distribution for the Amalthea ring derived from our in-situ measurements for the small grains agrees very well with the one obtained from images for large grains. Our analysis shows that particles contributing most to the optical cross-section are about 5 μm in radius, in agreement with imaging results. The measurements indicate a large drop in particle flux immediately interior to Thebe’s orbit and some detected particles seem to be on highly-tilted orbits with inclinations up to 20°. Finally, the faint Thebe ring extension was detected out to at least 5R_J, indicating that grains attain higher eccentricities than previously thought. The drop interior to Thebe, the excess of submicron grains at Amalthea, and the faint ring extension indicate that grain dynamics is strongly influenced by electromagnetic forces. These findings can all be explained by a shadow resonance as detailed by Hamilton and Krüger [Hamilton, D.P., Krüger, H., 2008. Nature 453, 72-75].     

沙尘暴垂直输运的两相流理论Ⅰ:气块模式

沙尘暴是风蚀荒漠化中的一种天气现象,其形成受到两方面因素的共同影响:(1)自然因素,包括大风、降水减少及沙源;(2)人类活动因素,人类活动因素是指人类在发展经济过程中对植被的破坏以后,导致沙尘暴爆发频率数增加.沙尘暴已经成为中国西北、华北地区严重的气候灾害,而对沙尘的研究主要集中在起沙问题与沙尘沉降的问题,在理论上对前者研究较多,而对后者的研究则比较缺乏.假设空气块中带有沙尘,沙尘颗粒很小,随空气一起运动,可不计沙尘Stockes末速度,这样由空气和沙尘组成两相流.在两相流情况下,分析了均匀环境和非均匀环境条件下沙尘沉降的条件和速率.通过分析得到在均匀背景场下有利于沙尘沉降的条件为大的初始沙尘浓度扰动与小的初始温度扰动.进一步考虑更为真实的环境场,模式给出3种特征沉降区域:(1)速降区,沉降速率较快;(2)缓降区,沙尘先上升后下降,沉降时间较长;(3)波动区,沙尘在空气中不断地上下波动,此时很难判断沙尘何时沉降,取决于地面状况.同时也分析了沙尘不断上扬的背景条件.     

北京两次沙尘污染过程中PM2.5浓度变化特征

利用北京市空气质量监测数据和气象资料,对2013年2月28日和3月9日两次沙尘污染过程PM2.5(空气动力学当量直径小于等于2.5μm的颗粒物,即细颗粒物)、PM10(空气动力学当量直径小于等于10μm的颗粒物,即可吸入颗粒物)浓度及PM2.5浓度/PM10浓度比值的变化特征进行了分析,研究结果表明:(1)沙尘开始影响北京时,PM2.5与PM10浓度表现出反位相变化,PM10浓度在两次沙尘过程中2 h内分别上升50.8%与202.4%,最高达800μg m-3以上;PM2.5浓度分别下降58.3%与50.9%,直至下降至35μg m-3以下,PM2.5有明显改善现象。(2)虽然PM2.5浓度在沙尘到达前有缓升的迹象,但沙尘抵达后,PM2.5浓度持续快速下降,PM2.5浓度/PM10浓度比值由沙尘影响前的0.75以上降至0.25以下。沙尘影响前,PM2.5日均值均超过150μg m-3,北京地区处于重度污染水平。这说明沙尘来临前以人为污染为主,主要由细粒子"贡献",沙尘来临后的空气污染,主要由巨、大粒子的沙尘"贡献"。