乌鲁木齐霾天气PM10单颗粒物理化学特征

为了解乌鲁木齐冬季污染天气形成过程中大气颗粒物化学组分的变化,探讨霾天气快速形成的主要原因,应用扫描电镜/X射线能谱仪(SEM/EDX)对2013年2月乌鲁木齐东南郊一次典型霾天和正常天气所采集的大气颗粒物(PM₁₀)样品进行了微观形貌和化学组成的对比分析。结果表明:伴随着霾形成过程细粒子浓度呈现急剧上升趋势,PM_1.0/PM₁₀比值高达0.77。SEM/EDX观测显示,霾天形成前后,PM₁₀的形态结构和元素组成存在较明显的差异,霾天规则的石膏颗粒占规则颗粒的71.1%,明显高于正常天气,表明大气颗粒物的硫化现象比较普遍,大量硅铝酸盐飞灰说明采样点周边有较明显的燃煤源输送;二次无机颗粒组成主要为硫酸盐颗粒,由正常天气的16.1%增加到24.6%,高浓度硫酸盐与乌鲁木齐东南郊此次霾形成有密切的联系。     

Denudation and retreat of the Serra do Mar escarpment in southern Brazil derived from in situ‐produced 10Be concentration in river sediment

The Serra do Mar escarpment, located along the southeastern coast of Brazil, is a high‐elevation passive margin escarpment. This escarpment evolved from the denudation of granites, migmatites and gneisses. The granites outcrop in the form of a ridge along the escarpment crest, due to its differential erosion (‘sugarloaf’ hills) from the surrounding lithologies. Several studies suggest that the passive margin escarpments are actively retreating toward the interior of the continent. However, no prior study has calculated the long‐term denudation rates of Serra do Mar to test this hypothesis. In this study, we measured the in situ‐produced ¹⁰Be concentration in fluvial sediments to quantify the catchment‐wide long‐term denudation rates of the Serra do Mar escarpment in southern Brazil. We sampled the fluvial sediments from ten watersheds that drain both sides of the escarpment. The average long‐term denudation rate of the oceanic side is between 2.1‐ and 2.6‐fold higher than the rate of the continental side: 26.04 ± 1.88 mm ka^‐1 (integrating over between 15.8 ka^‐1 and 46.6 ka^‐1) and 11.10 ± 0.37 mm ka^‐1 (integrating over between 52.9 ka^‐1 and 85.4 ka^‐1), respectively. These rates indicate that the coastal base level is controlling the escarpment retreat toward the continental high lands, which is consistent with observations made at other high‐elevation passive margins around the globe. The results also demonstrate the differential erosion along the Serra do Mar escarpment in southern Brazil during the Quaternary, where drainages over granites had lower average denudation rates in comparison with those over migmatites and gneisses. Moreover, the results demonstrate that the ocean‐facing catchments have been eroded more intensely than those facing the continent. The results also reveal that drainage over the granites decreases the average denudation rates of the ocean‐facing catchments and the ‘sugarloaf’ hills therefore are natural barriers that slowly retreat once they are exhumed. Copyright © 2013 John Wiley & Sons, Ltd.     

Transient sediment supply in a high‐altitude Alpine environment evidenced through a 10Be budget of the Etages catchment (French Western Alps)

Although beryllium‐10 (¹⁰Be) concentrations in stream sediments provide useful synoptic views of catchment‐wide erosion rates, little is known on the relative contributions of different sediment supply mechanisms to the acquisition of their initial signature in the headwaters. Here we address this issue by conducting a ¹⁰Be‐budget of detrital materials that characterize the morphogenetic domains representative of high‐altitude environments of the European Alps. We focus on the Etages catchment, located in the Ecrins‐Pelvoux massif (southeast France), and illustrate how in situ ¹⁰Be concentrations can be used for tracing the origin of the sand fraction from the bedload in the trunk stream. The landscape of the Etages catchment is characterized by a geomorphic transient state, high topographic gradients, and a large variety of modern geomorphic domains ranging from glacial environments to scarcely vegetated alluvial plains. Beryllium‐10 concentrations measured in the Etages catchment vary from ~1 × 10⁴ to 4.5 × 10⁵ atoms per gram quartz, while displaying consistent ¹⁰Be signatures within each representative morphogenetic unit. We show that the basic requirements for inferring catchment‐wide denudation from ¹⁰Be concentration measurements are not satisfied in this small, dynamic catchment. However, the distinct ¹⁰Be signature observed for the geomorphic domains can be used as a tracer. We suggest that a terrestrial cosmogenic nuclide (TCN) budget approach provides a valuable tool for the tracing of material origin in basins where the ‘let nature do the averaging’ principles may be violated. Copyright © 2013 John Wiley & Sons, Ltd.     

祁连山疏勒河上游多年冻土区高寒草甸土壤CO2通量特征

研究青藏高原多年冻土区高寒草甸土壤CO₂通量有助于准确估算该区域的土壤CO₂排放, 对认识高原土壤碳循环及其对全球气候变化的响应具有重要意义. 利用静态箱-气相色谱法和LI-8100土壤CO₂通量自动测量系统对疏勒河上游多年冻土区高寒草甸土壤CO₂通量进行了定期观测, 结合气象和土壤环境因子进行了分析. 结果表明: 整个观测期高寒草甸土壤表现为CO₂的源, 土壤CO₂通量的日变化范围为2.52～532.81 mg·m^-2·h^-1. 土壤CO₂年排放总量为1 429.88 g·m^-2, 年均通量为163.23 mg·m^-2·h^-1; 其中, CO₂通量与空气温度和相对湿度、活动层表层2 cm、10 cm、20 cm、30 cm 土壤温度、含水量和盐分均显著相关. 2 cm土壤温度、空气温度和总辐射、空气温度、2 cm土壤盐分分别是影响活动层表层2 cm土壤完全融化期、冻结过程期、完全冻结期、融化过程期土壤CO₂通量的最重要因子. 在完全融化期、冻结过程期和整个观测期, 拟合最佳的温度因子变化分别能够解释土壤CO₂通量变化的72.0%、82.0%和38.0%, 对应的Q₁₀值分别为1.93、6.62和2.09. 冻融期(含融化过程期和冻结过程期)和完全冻结期的土壤CO₂排放量分别占年排放总量的15.35%和11.04%, 在年排放总量估算中不容忽视.     

地表岩石侵蚀速率对宇生核素暴露测年影响的研究

利用原地生宇生核素测定暴露年代时,通常会假设地貌体侵蚀速率为0。研究表明,该假设会低估地貌体的真实暴露年代。搜集2009~2012年全球不同区域56个岩石样品的宇生核素¹⁰Be测年数据,探讨侵蚀速率为0对于侵蚀速率为0.5、1以及2 mm/ka的样品,在不同暴露尺度上对暴露年代计算的影响幅度。结果表明,对于1×10⁴a尺度的样品暴露年代可能低估约0.5%,1%,2%;对于10×10⁴a尺度的样品可能低估约5%,7%,20%;对于50×10⁴a尺度的样品可能低估约40%,70%甚至100%以上。     

兰州市大气气溶胶的特征及其对呼吸道疾病的影响

根据2000年6月至2001年5月兰州市大气气溶胶的监测资料,分析了兰州市大气气溶胶的浓度、尺度谱分布及其年、月、日变化规律,进而探讨了大气气溶胶对人体舒适度的影响,分析了大气气溶胶浓度与呼吸道疾病发病人数之间的关系。结果表明:PM10月均浓度与同期呼吸道疾病月发病人数的变化趋势基本一致,两者呈显著性正相关;当PM10日均浓度明显升高后1～2 d,呼吸道疾病发病人数也随之增多。     

内蒙古一次强沙尘暴过程综合观测分析

利用高空、地面常规观测资料和内蒙古沙尘暴监测站的沙尘暴器测资料,对2010年3月19～20日一次强沙尘暴天气过程进行了综合观测分析.结果表明:本次沙尘暴发生前,大气层结稳定并不利于对流的发展.但在700 hPa至500 hPa的强冷平流与850 hPa以下层次的平流差异有利于温度垂直递减率增大,强冷平流的作用使其中心以下层次形成热力不稳定层结,是沙尘暴发生的有利层结条件.当干对流风暴发生并形成沙尘暴天气时,不稳定能量释放,使该层大气趋于中性层结即混合层,混合层可能是其间的一个平衡态.对流层中低层冷平流的强度、位置和层次,一定程度上影响着混合层的厚度和沙尘暴的强度.过程中混合层以下气层温度下降的比较快,加之沙尘暴顶层短波辐射有增温效果,在混合层顶(约500 hPa处)出现逆温盖.强冷空气活动是引发沙尘暴天气的主要原因,沙尘暴天气的发生伴随着地面剧烈降温,相对湿度骤降,气压涌升,地面风速直接影响沙尘暴强度.可吸入颗粒物(PM10)浓度能更加精细的反映和描述沙尘暴强度的变化.粒子散射系数的变化趋势和PM10浓度的变化趋势非常一致,沙尘暴阶段,散射系数基本在1000Mm-1以上,达到强沙尘暴强度阶段,散射系数基本在2000Mm-1以上.     

基于MODIS的祁连山区积雪时空变化特征

利用2000-2003年日资料经8 d合成的500 m分辨率MODIS卫星反演积雪资料和数字高程模型, 借助于GIS空间分析技术, 以积雪频率和积雪盖度为监测指标, 研究分析了祁连山区整体的积雪空间分布状况及其年内变化特征, 地形对积雪的分布和季节变化的影响. 结果表明: 祁连山区的积雪分布极不均匀, 积雪主要沿山系走向成条带状分布, 呈现西段多, 东段次之, 中部和南部少, 山脊多, 山谷少的特征, 且海拔越高、 山势越陡、阴坡积雪的范围越大、持续时间越久. 累积降雪时间, 就全区而言为9月至翌年5月, 但不同高度、坡度和坡向带有所差别. 海拔4 000 m以上区域存在春、秋季两个时段的积雪补给, 而海拔4 000 m以下仅有中秋至中冬一个时段的积雪补给;坡度较平缓的区域冬季和春季为主要积雪补给期, 而坡度较陡的区域则为秋季和春季;平地和南坡积雪补给主要发生在冬季和春季, 而其它坡向为春季和秋季.     

2004年春季沙尘天气对和田市空气质量的影响

利用沙尘暴监测网数据、常规气象资料以及MICAPS系统环流形势资料,对和田市2004年春季沙尘天气产生的污染进行了详细的对比分析。研究结果表明：和田市春季污染相当严重,主要以沙尘污染为主。整个春季79％时间API（环境污染指数）指数均达到500,且45％时间可吸入颗粒物PM10在TSP巾的浓度比例达50％。不同天气系统对和田市空气的污染贡献不同。从东路影响和田市的天气系统、高压底部型地面系统和浮尘天气所造成空气污染相当严重。其余天气系统和天气现象所产生的污染较小。     

Could CoRoT-7b and Kepler-10b be remnants of evaporated gas or ice giants?

We present thermal mass loss calculations over evolutionary time scales for the investigation if the smallest transiting rocky exoplanets CoRoT-7b (∼1.68R_Earth) and Kepler-10b (∼1.416R_Earth) could be remnants of an initially more massive hydrogen-rich gas giant or a hot Neptune-class exoplanet. We apply a thermal mass loss formula which yields results that are comparable to hydrodynamic loss models. Our approach considers the effect of the Roche lobe, realistic heating efficiencies and a radius scaling law derived from observations of hot Jupiters. We study the influence of the mean planetary density on the thermal mass loss by placing hypothetical exoplanets with the characteristics of Jupiter, Saturn, Neptune, and Uranus to the orbital location of CoRoT-7b at 0.017 AU and Kepler-10b at 0.01684 AU and assuming that these planets orbit a K- or G-type host star. Our findings indicate that hydrogen-rich gas giants within the mass domain of Saturn or Jupiter cannot thermally lose such an amount of mass that CoRoT-7b and Kepler-10b would result in a rocky residue. Moreover, our calculations show that the present time mass of both rocky exoplanets can be neither a result of evaporation of a hydrogen envelope of a “Hot Neptune” nor a “Hot Uranus”-class object. Depending on the initial density and mass, these planets most likely were always rocky planets which could lose a thin hydrogen envelope, but not cores of thermally evaporated initially much more massive and larger objects.