Arsenic Speciation in Lichens and in Coarse and Fine Airborne Particulate Matter by HPLC–UV–HG–AFS     

M. M. Farinha  Z. Šlejkovec  J. T. van Elteren  H. Th. Wolterbeek  M. C. Freitas 《Journal of Atmospheric Chemistry》2004,49(1-3):343-353

A three-step sequential extraction procedure with Milli-Q, CaCl₂ and H₃PO₄ was applied for extraction of arsenic species in lichen transplants and airborne particulate matter (fine and coarse fractions). The samples used in this work were collected in 1994–1995 near coal-fired power plants. Both transplant lichens and airborne particulate matter were submitted to the same environment simultaneously. Arsenic species identification and quantification was performed by HPLC–UV–HG–AFS. Inorganic forms of arsenic (arsenite and arsenate) were present in significant amounts in most of the samples. Only in lichens also organic forms of arsenic (monomethyl arsonic acid and dimethyl arsinic acid) were identified which may indicate biotransformation of inorganic arsenic.  相似文献   

基于欧洲中心细网格预报资料和观测资料的浙江省春夏降水性质分类指标     

王霁吟  陈懿妮  孙长  王丽颖  俞佩 《气候与环境研究》2018,23(5):543-550

利用浙江省2004~2013年3~8月Micaps（气象信息综合分析处理系统）地面填图数据和T-logP数据研究杭州、衢州和台州三市的阵雨和雷雨个例,同时选取能表征雷雨并能区分阵雨与雷雨的气象预报因子:对流有效位能、850 hPa与500 hPa的温差、K指数、地面2 m温度,用临近探空的分析方法和决策树的分类方法初步建立了一个适用于浙江省春夏季降水性质分类指标。利用欧洲中心（ECMWF）细网格预报资料,对历史样本和2016年春、夏季分别作了检验。结果表明:除去有降水预报误差个例后,指标TS（Threat Score）评分超过0.53,雷雨阵雨综合命中率达到71%,空报率阵雨（10%）小于雷雨（43%）,在不同地区和季节稍有区别;同时对浙江省2016年春夏两次典型大范围阵雨雷雨过程进行预报,效果很好。此方法不仅可以依据预报数据在短期内做出精细化降水性质分类预报,在中长期预报上也有表现力。  相似文献   

一次降水性积层混合云系的微物理特征分析     

张佃国  樊明月  龚佃利  张洪生 《南京气象学院学报》2010,33(4):496-503

利用山东省2007年10月27日1架次机载粒子测量系统（Particles Measuring System,PMS）积层混合云探测资料,分析了云中粒子浓度和尺度、液态含水量,以及小云滴和大云滴谱的垂直分布特征,比较了催化前后云微物理特征的变化。结果表明,催化前,云层中小云滴谱型为单峰,谱宽随高度增加先变窄后变宽,大云滴谱型在云低层为单峰,中高层为双峰谱,谱宽随高度增加先变宽后变窄,并且没有探测到降水粒子。催化后,小云滴尺度在低层减小、高层增加,整层液态水含量减小;大云滴浓度增加,尺度增大,出现降水粒子,固态粒子类型增多。在3 700~4 000 m高度层内小于10μm粒子明显增加,说明凝结过程比较明显,并且10~27.5μm粒子开始出现,启动了云滴的碰并机制。小云滴谱变化较小,基本为单峰谱,但在较大云滴处谱型略有起伏,在3 000m和3 300m高度的谱宽增宽。大云滴粒子谱有较大的变化,低层变成双峰谱,谱宽最宽可达650μm,中高层为双峰或多峰,峰值从小值向较大值移动。2D-P探头在催化云高层探测到降水粒子,谱型呈单调下降形态,谱宽最大为600μm。  相似文献   

On the formation and growth of atmospheric nanoparticles   总被引：2，自引：0，他引：2  

Markku Kulmala  Veli-Matti Kerminen 《Atmospheric Research》2008,90(2-4):132-ICNAA07

In this paper we summarize recent experimental, theoretical and observational results on the formation and growth of atmospheric nanoparticles. During the last years significant progress has occurred to explain atmospheric nucleation and initial steps of the growth. Due to climatic and health effects of fine and ultrafine particles the formation and growth of new aerosol particles is of growing interest. The question “How and under which conditions does the formation of new atmospheric aerosol particles take place?” has exercised the minds of scientists since the time of John Aitken, who in the late 1880s built the first apparatus to measure the number of dust and fog particles. However, only during the last 15–20 years has the measurement technology developed to such a level that size distributions of nanometer-size particles and concentrations of gases participating in particle formation can be measured in the atmosphere. Also from a theoretical point of view atmospheric nucleation mechanisms have not been resolved: several mechanisms such as ion-induced (or ion mediated) nucleation, ternary and kinetic (barrier-less) nucleation have been suggested. In the most recent theory, the activation of existing neutral and/or ion clusters has been suggested.  相似文献   

0679香山局地大暴雨的中小尺度天气分析   总被引：22，自引：3，他引：19       下载免费PDF全文

郭虎  段丽  杨波  卞素芬  李靖 《应用气象学报》2008,19(3):265-275

利用Doppler雷达、地面自动站、Profile垂直风廓线及GPS水汽分布等多种新型探测资料, 对2006年7月9日夜间发生在北京西郊香山附近的局地大暴雨天气的影响系统和γ-中尺度强降雨落区形成的动力机理进行了精细分析。对雷达等本地多种探测资料的精细研究表明:地形辐合回波带是造成这次过程的主要影响系统。地形辐合回波带上中气旋回波块的滚动更迭是大暴雨落区形成的直接原因; 近地面辐合对大暴雨落区强降雨的发生具有重要作用。大暴雨落区形成阶段近地面3种辐合同时存在:平原东南风与山区偏北风风向切变辐合、平原东南风在山脉阻挡作用下的抬升辐合、大暴雨落区中心的γ-中尺度气旋性辐合。研究还表明:山前近地面地形辐合扰动, 向上传播, 引发边界层扰动的动力过程是香山大暴雨落区形成的主要动力源, 而来自东南方向近地面层的暖湿平流为大暴雨提供了有效的水汽和能量。  相似文献   

High-energy particle acceleration and production of ultra-high-energy cosmic rays in the giant lobes of Centaurus A     

M. J. Hardcastle  C. C. Cheung  I. J. Feain  &#;. Stawarz 《Monthly notices of the Royal Astronomical Society》2009,393(3):1041-1053

The nearby radio galaxy Centaurus A is poorly studied at high frequencies with conventional radio telescopes because of its very large angular size, but is one of a very few extragalactic objects to be detected and resolved by the Wilkinson Microwave Anisotropy Probe ( WMAP ). We have used the five-year WMAP data for Cen A to constrain the high-frequency radio spectra of the 10° giant lobes and to search for spectral changes as a function of position along the lobes. We show that the high-frequency radio spectra of the northern and southern giant lobes are significantly different: the spectrum of the southern lobe steepens monotonically (and is steeper further from the active nucleus) whereas the spectrum of the northern lobe remains consistent with a power law. The inferred differences in the northern and southern giant lobes may be the result of real differences in their high-energy particle acceleration histories, perhaps due to the influence of the northern middle lobe, an intermediate-scale feature which has no detectable southern counterpart. In light of these results, we discuss the prospects for Fermi Gamma-ray Space Telescope detections of inverse-Compton emission from the giant lobes and the lobes' possible role in the production of the ultra-high-energy cosmic rays (UHECR) detected by the Pierre Auger Observatory. We show that the possibility of a Fermi detection depends sensitively on the physical conditions in the giant lobes, with the northern lobe more likely to be detected, and that any emission observed by Fermi is likely to be dominated by photons at the soft end of the Fermi energy band. On the other hand, we argue that the estimated conditions in the giant lobes imply that UHECRs can be accelerated there, with a potentially detectable γ-ray signature at TeV energies.  相似文献   

Dark matter annihilation at cosmological redshifts: possible relic signal from annihilation of weakly interacting massive particles     

A. N. Baushev 《Monthly notices of the Royal Astronomical Society》2009,398(2):783-789

We discuss the possibility of observing the products of the dark matter annihilation that was going on in the early Universe. Of all the particles that could be generated by this process, we consider only photons, as they are both uncharged and easily detectable. The younger the Universe was, the higher the dark matter concentration n and the annihilation rate (proportional to n ²) were. However, the emission from the very early Universe cannot reach us because of the opacity. The main part of the signal was generated at the moment the Universe had just become transparent for the photons produced by the annihilation. Thus, the dark matter annihilation in the early Universe should have created a sort of relic emission. We obtain its flux and the spectrum.
If weakly interacting massive particles (WIMPs) constitute dark matter, it is shown that we may expect an extragalactic gamma-ray signal in the energy range 0.5–20 MeV with a maximum near 8 MeV. We show that an experimentally observed excess in the gamma-ray background at 0.5–20 MeV could be created by the relic signal from the annihilation of WIMPs only if the dark matter structures in the Universe had appeared before the Universe became transparent for the annihilation products  ( z ≃ 300)  . We discuss in more detail physical conditions whereby this interpretation could be possible.  相似文献   

On the origin of the 511-keV emission in the Galactic Centre     

Reba M. Bandyopadhyay  Joseph Silk  James E. Taylor  Thomas J. Maccarone 《Monthly notices of the Royal Astronomical Society》2009,392(3):1115-1123

Diffuse 511-keV line emission, from the annihilation of cold positrons, has been observed in the direction of the Galactic Centre for more than 30 yr. The latest high-resolution maps of this emission produced by the SPI instrument on INTEGRAL suggest at least one component of the emission is spatially coincident with the distribution of ∼70 luminous, low-mass X-ray binaries detected in the soft gamma-ray band. The X-ray band, however, is generally a more sensitive probe of X-ray binary populations. Recent X-ray surveys of the Galactic Centre have discovered a much larger population (>4000) of faint, hard X-ray point sources. We investigate the possibility that the positrons observed in the direction of the Galactic Centre originate in pair-dominated jets generated by this population of fainter accretion-powered X-ray binaries. We also consider briefly whether such sources could account for unexplained diffuse emission associated with the Galactic Centre in the microwave (the Wilkinson Microwave Anisotropy Probe 'haze') and at other wavelengths. Finally, we point out several unresolved problems in associating Galactic Centre 511-keV emission with the brightest X-ray binaries.  相似文献   

A kinetic approach to cosmic-ray-induced streaming instability at supernova shocks   总被引：1，自引：0，他引：1  

E. Amato  P. Blasi 《Monthly notices of the Royal Astronomical Society》2009,392(4):1591-1600

We show that a purely kinetic approach to the excitation of waves by cosmic rays in the vicinity of a shock front leads to predict the appearance of a non-Alfvénic fast-growing mode which has the same dispersion relation as that previously found by Bell in 2004 by treating the plasma in the magnetohydrodynamic approximation. The kinetic approach allows us to investigate the dependence of the dispersion relation of these waves on the microphysics of the current which compensates the cosmic ray flow. We also show that a resonant and a non-resonant mode may appear at the same time and one of the two may become dominant on the other depending on the conditions in the acceleration region. We discuss the role of the unstable modes for magnetic field amplification and particle acceleration in supernova remnants at different stages of the remnant evolution.  相似文献   

Some properties of synchrotron radio and inverse-Compton gamma-ray images of supernova remnants     

O. Petruk  V. Beshley  F. Bocchino  S. Orlando 《Monthly notices of the Royal Astronomical Society》2009,395(3):1467-1475

The synchrotron radio maps of supernova remnants (SNRs) in a uniform interstellar medium and interstellar magnetic field (ISMF) are analysed, allowing for different 'sensitivity' of the injection efficiency to the obliquity of the shock. The very-high-energy γ-ray maps arising from inverse Compton processes are also synthesized. The properties of images in these different wavelength bands are compared, with particular emphasis on the location of the bright limbs in bilateral SNRs. Recent High-Energy Stereoscopic System (HESS) observations of SN 1006 show that the radio and inverse Compton γ-ray limbs coincide, and we found that this may happen if (i) injection is isotropic but the variation of the maximum energy of electrons is rather fast to compensate for differences in the magnetic field, or (ii) the obliquity dependence of injection (either quasi-parallel or quasi-perpendicular) and the electron maximum energy are strong enough to dominate the magnetic field variation. In the latter case, the obliquity dependences of the injection and the maximum energy should not be opposite. We argue that the position of the limbs alone, and even their coincidence in radio, X-rays and γ-rays, as discovered by HESS in SN 1006, cannot be conclusive as regards the dependence of the electron injection efficiency, the compression/amplification of the ISMF and the electron maximum energy on the obliquity angle.  相似文献