An investigation of the SO2 content of the venusian mesosphere using SPICAV-UV in nadir mode

Using the SPICAV-UV spectrometer aboard Venus Express in nadir mode, we were able to derive spectral radiance factors in the middle atmosphere of Venus in the 170-320 nm range at a spectral resolution of R ? 200 during 2006 and 2007 in the northern hemisphere. By comparison with a radiative transfer model of the upper atmosphere of Venus, we could derive column abundance above the visible cloud top for SO₂ using its spectral absorption bands near 280 and 220 nm. SO₂ column densities show large temporal and spatial variations on a horizontal scale of a few hundred kilometers. Typical SO₂ column densities at low latitudes (up to 50°N) were found between 5 and 50 μm-atm, whereas in the northern polar region SO₂ content was usually below 5 μm-atm. The observed latitudinal variations follow closely the cloud top altitude derived by SPICAV-IR and are thought to be of dynamical origin. Also, a sudden increase of SO₂ column density in the whole northern hemisphere has been observed in early 2007, possibly related to a convective episode advecting some deep SO₂ into the upper atmosphere.     

The 1.10- and 1.18-μm nightside windows of Venus observed by SPICAV-IR aboard Venus Express

Observations of the 1.10- and 1.18-μm nightside windows by the SPICAV-IR instrument aboard Venus Express were analyzed to characterize the various sources of gaseous opacity and determine the H₂O mole fraction in the lower atmosphere of Venus. We showed that the line profile model of Afanasenko and Rodin (Afanasenko, T.S., Rodin, A.V. [2007]. Astron. Lett. 33, 203–210) underestimates the CO₂ absorption in the high-wavelength wing of the 1.18-μm window and we derived an empirical lineshape that matches this wing well. An additional continuum opacity is required to reproduce the variation of the 1.10- and 1.18-μm radiances with surface elevation as observed by the VIRTIS-M instrument aboard Venus Express. A constant absorption coefficient of 0.7 ± 0.2 × 10⁻⁹ cm⁻¹ am⁻² best reproduces the observed variation. We compared spectra calculated with different CO₂ and H₂O line lists. We found that the CDSD line list lacks the 5ν₁ + ν₃ series of CO₂ bands, which provide significant opacity in Venus’ deep atmosphere, and we have constructed a composite line list that best reproduces the observations. We also showed for the first time that HDO brings significant absorption at 1140–1190 nm. Using the best representation of the atmospheric opacity we could reach, we retrieved a water vapor mole fraction of ppmv, pertaining to the altitude range 5–25 km. Combined with previous measurements in the 1.74- and 2.3-μm windows, this result provides strong evidence for a uniform H₂O profile below 40 km, in agreement with chemical models.     

Saturn’s zonal wind profile in 2004-2009 from Cassini ISS images and its long-term variability

Five years of Cassini Imaging Science Subsystem images, from 2004 to 2009, are analyzed in this work to retrieve global zonal wind profiles of Saturn’s northern and southern hemispheres in the methane absorbing bands at 890 and 727 nm and in their respective adjacent continuum wavelengths of 939 and 752 nm. A complete view of Saturn’s global circulation, including the equator, at two pressure levels, in the tropopause (60 mbar to 250 mbar with the MT filters) and in the upper troposphere (from ∼350 mbar to ∼500 mbar with the CB filter set), is presented. Both zonal wind profiles (available at the Supplementary Material Section), show the same structure but with significant differences in the peak of the eastward jets and the equatorial region, including a region of positive vertical shear symmetrically located around the equator between the 10° < |φ_c| < 25° where zonal velocities close to the tropopause are higher than at 500 mbar. A comparison of previously published zonal wind sets obtained by Voyager 1 and 2 (1980-1981), Hubble Space Telescope, and ground-based telescopes (1990-2004) with the present Cassini profiles (2004-2009) covering a full Saturn year shows that the shape of the zonal wind profile and intensity of the jets has remained almost unchanged except at the equator, despite the seasonal insolation cycle and the variability of Saturn’s emitted power. The major wind changes occurred at equatorial latitudes, perhaps following the Great White Spot eruption in 1990. It is not evident from our study if the seasonal insolation cycle and its associated ring shadowing influence the equatorial circulation at cloud level.     

闽南沿海地区不同日观测次数大气稳定度的对比

本文通过地处闽南沿海地区崇武气候站不同日观测次数大气稳定度的对比分析表明 :采用 8个时次和 4个时次观测记录所统计的稳定度频数 ,误差较小(与 2 4个时次比较 ,下同 ) ,对重要结论无大影响 ,能够较准确地描述大气稳定度的状况和特征 ;而采用 3个时次观测资料分析 ,其误差大 ,甚至导致相反的结果 ,实际应用时必须慎重。     

环境空气中的气溶胶污染的影响分析

环境空气中气溶胶粒子是由极性气体凝聚而成,呈三峰型分布.对其空气中溶胶粒子,特别是可吸入粒子的成分,气溶胶态、粒径大小、浓度等对人体健康危害进行了分析研究.     

触发重庆山洪灾害的典型环流和影响系统分析

通过对触发重庆山洪灾害的31次区域性暴雨的特点以及产生重庆区域性暴雨的典型大气环流形势和主要影响系统的统计分析,结果表明:(1)重庆山洪灾害主要是强降水引起的滑坡、局部泥石流和小溪流的洪涝等灾害,其危害极大;(2)诱发重庆山洪灾害的典型区域性强降水主要出现在5~9月,其中7月出现频率最大;(3)绝大部分区域性强降水过程产生前,在500 hPa中、高纬地区上空形成两脊一槽型(占52%)或两槽一脊型的环流形势(占42%);(4)高原槽(高原切变)、高原涡、副热带高压、西南涡、低空急流、地面冷锋等为其主要影响系统。     

A photoelectric detector for the measurement of photolysis frequencies of ozone and other atmospheric molecules

Photoelectric detectors for the measurement of photolysis frequencies of different trace gases in the atmosphere are described. They exhibit uniform response characteristics over one hemisphere (2 sr) and wavelength characteristics closely matched to those of the photolysis frequencies J _O1D, J _NO2, and J _NO3, respectively. Absolute calibration of the J _O1D detector was performed by chemical actinometry with an accuracy of ±16 percent. Simultaneous measurements of J _NO2 and J _O1D are presented.     

沙尘气溶胶对西北地区植被遥感的影响分析

选取扬沙—浮尘天气发生中、后的对地观测卫星EOS-MODIS数据,利用6S辐射传输模式对该卫星资料进行大气订正,分析了沙尘气溶胶对沙尘多发区的西北地区植被指数(VI)遥感的影响。结果表明,与晴空天气得到的反射率相比,沙尘使红光通道反射率ρ1、近红外通道反射率ρ2和蓝光通道反射率ρ3均增加,归一化植被指数NDVI有不同程度的降低,降低最大值为0.246。抗大气植被指数ARVI也有所降低,降低最大值为0.231。应用晴空天气条件下的资料,建立了西北干旱区ARVI与NDVI之间的线性关系,并证明了在沙尘天气条件下,利用ARVI计算NDVI的方法,所得的结果较好。     

低纬高原城市区域冬季晴天不同波长辐射的特征

利用低纬高原城市昆明城区内外不同波长辐射的实测资料,分析了研究得较少的城区内外不同波长辐射的分布特征、变化规律及其差异,主要结果如下：（１）城内因受周围大气环境质量的影响,各波长辐射量的变化离散性大于城外;不同波长辐射的绝对量和相对量（城内外比值）大多是城内小于城外,且以大气污染严重的午前差异显著。（２）低纬高原城市区域,冬季晴好天气时午前、午后不同波长射占总辐射的百分率存在差异;城内外各辐射的百     

FGOALS_gg1.1极地气候模拟

对中国科学院大气物理研究所大气科学和地球流体力学数值模拟国家重点实验室发展的气候系统模式FGOALS_g1.1的极地气候模拟现状进行了较为全面的评估.结果表明,FGOALS_g1.1对南北极海冰的主要分布特征、季节变化和年代际变化趋势具有一定的模拟能力.但也注意到,与观测相比,模式存在以下几方面的问题:(1)模拟的海冰总面积北极偏多,而南极偏少.北极,北大西洋海冰全年明显偏多;夏季,西伯利亚沿海海冰偏多,而波弗特海海冰偏少.南极,威德尔海和罗斯海冬季海冰偏少.南北极海冰边缘都存在异常的较大范围密集度很小的碎冰区,夏季尤为显著.(2)海冰流速在南北极海冰边缘和南极大陆沿岸附近较大.北极,模式没能模拟出波弗特涡流,并且由于模式网格中北极点的处理问题,造成其附近错误的海冰流场及厚度分布.这些海冰偏差与模式模拟的大气和海洋状况有着密切的联系.进一步分析表明,FGOALS_g1.1模拟的冰岛低压和南极绕极西风带明显偏弱,其通过大气环流和海表面风应力影响向极地的热量输送,在很大程度上导致上述的海冰偏差.此外,耦合模式中大气-海冰-海洋的相互作用可以放大子模式中的偏差.