夏季长江中下游和华南两类雨型的环流特征及预测信号

利用中国南方66站降水观测资料和NCEP/NCAR再分析资料,采用经验正交函数分解（EOF）、合成分析和相关分析等方法,对夏季长江中下游和华南两类雨型进行了划分,对比分析了两类雨型同期大气环流和前期海温及环流的差异,以探讨两类雨型的形成机制及前期预测信号。结果表明:20世纪80年代之前华南型出现的频次较高,之后长江中下游型出现频次增多;长江中下游型年西太平洋副热带高压（副高）偏强偏西偏南,东亚夏季风（EASM）偏弱,副热带西风急流位置偏南,乌拉尔山阻塞高压（乌阻）和鄂霍次克海阻塞高压（鄂阻）较强,欧亚中高纬以经向环流为主,冷暖空气在长江中下游辐合,导致长江中下游降水偏多;华南型年大气环流与长江中下游型年大体相反,登陆华南的台风偏多,冷暖空气在华南地区辐合,导致华南地区降水偏多;其中副高的脊线位置和中高纬阻塞强弱是长江中下游型和华南型形成的关键因素。两类雨型前期海温分析表明,长江中下游型年,前冬赤道中东太平洋和印度洋偏暖,为典型的东部型El Ni?o,副热带南印度洋偶极子（SIOD）呈负位相,春季El Ni?o衰减,SIOD负位相也减弱,但印度洋持续增暖;华南型年,前冬和春季的海洋演变与长江中下游型年大体相反;关键区域海温与长江中下游夏季降水（YRR）和华南夏季降水（SCR）的年际关系存在年代际变化,YRR和SCR与前冬Ni?o3.4指数、SIOD指数和春季热带印度洋全区一致海温模态（IOBW）指数的相关关系在80年代之后逐步减弱,这主要是由于这三个关键海温指数与EASM及副高脊线的相关关系在80年代之后逐步减弱;两类雨型前期大气环流差异分析表明,春季大气环流的差异性要比前冬显著,长江中下游型年,春季副高、南海副高、马斯克林高压（马高）、澳大利亚高压（澳高）均偏强,大西洋欧洲区极涡强度偏弱,北太平洋涛动（NPO）呈正位相;华南型年春季的关键环流系统异常不明显,仅大西洋欧洲区极涡强度偏强,NPO呈负位相。前期海温演变及春季大气环流关键系统的异常可以作为两类雨型年的一些预测信号。     

常压室温等离子体技术诱变选育鲅鱼抗氧化肽发酵菌株

鲅鱼(Spanish mackerel)加工后的废弃物富含蛋白质,为了提高蛋白质的利用率并减少环境污染,可以采用微生物发酵的方法酶解这部分蛋白质制取抗氧化活性肽。本实验室已经筛选出一株芽孢杆菌(Bacillus subtilis)Hy-2,以其发酵水产加工废弃物得到了具有较高抗氧化性的产物。为了进一步提高产物的抗氧化性,作者以该株产蛋白酶芽孢杆菌Hy-2为出发菌,采用常压室温等离子体(ARTP)诱变的方法筛选出1株突变菌Hy-23,以鲅鱼加工后的废弃物为原料,接种该突变菌株进行发酵,得到了具有一定抗氧化活性的发酵产物,酶解物总抗氧化活性提高了12.4%。经遗传稳定性测定,该芽孢杆菌突变株在传代8次之后其遗传稳定性仍然良好。     

利用卫星激光观测对大气折射模型的综合比较

利用3天22个测站的Lageos-1激光测距资料,解算出卫星的一条轨道,再利用此轨道和地面测站检验原有的大气折射模型.得到定轨常用的Marini(1973)模型以及Yan (1999)模型、UNSW932模型、Cfa2.2(1985)模型等的改正特点.     

Geogenic versus anthropogenic geochemical influence on trace elements contents in soils from the Milazzo Peninsula

Milazzo Peninsula soils and substrates are extremely variable, composed of acidic, mafic and ultramafic metamorphic rocks, carbonatic sedimentary rocks, and sometimes volcanic rocks, thus contributing to a mixed influence on their chemical composition. Moreover, the region is highly polluted due to atmospheric releases from anthropogenic activities, such as refinery industry. In addition, emissions of airborne particles from volcanic eruptions are also likely to fall to the ground and provide trace elements to the soils. The purpose of this study is to distinguish between anthropogenic and geogenic sources contributing to the concentrations of metals in soils by studying their distribution in major and trace elements in relation to substrates. As regards geogenic sources, the major elements composition of soils comes firstly from metamorphic rocks, secondly from carbonates, and to a minor extent from volcanic rocks. Enrichment factors calculations relative to substrate rocks, and using Th as reference element, show that the soils are enriched in As, Pb, Zn, and Ni. Rare earth elements (REEs) patterns normalized to substrate rocks exhibit enrichment in light REEs and a positive anomaly in Gd, indicating anthropogenic contributions in the soil composition. REE ratios and trace elements were plotted to investigate the relationships between anthropogenic sources and substrates in soils compositions. The graphs of La/Ni vs La/Gd and La/Ce vs La/Nd show that soils plot on a line toward substrate rocks on one side, and toward an end member which is represented by a spent catalyst and atmospheric particles emitted by refinery activities. Plots of La vs Cr, and V vs La show similar trends, whereas plots of Zn vs Ni and Pb vs V suggest that another end member, which is unidentified, contributes to soil enrichment in Zn and Pb. A binary mixing model applied to the most Zn enriched soil suggests that anthropogenic inputs from refinery emissions may have contributed to 16% of the anomalies in La/Gd. These results suggest that the trace element composition of Milazzo's peninsula soils partly bears the signature of atmospheric emissions of the refinery.     

大气压电离质谱及其用于超高纯气体分析研究进展

超高纯气体在工业生产中有非常重要的地位,如半导体工业中电子气的质量直接影响半导体器件的性能,百万分之几的微量杂质气体便可导致集成电路中元件存储信息量的减少。越来越高的气体纯度要求对分析方法及仪器的灵敏度提出了很大的挑战。大气压电离质谱(APIMS)由于可以在大气压条件下对杂质进行电离,并伴随高效的电离方式,因此具有极高的灵敏度,成为超高纯气体杂质分析中极为有效的技术手段,特别适合检测10^-9 mol/mol甚至10^-12 mol/mol浓度量级的气体杂质。APIMS采用电晕放电及⁶³Ni两种电离源,通常以电晕放电电离源为主,质量分析器常采用四极杆,同时为适应超高纯气体分析,APIMS配备了气体进样系统及可将标准气体稀释产生校正气体的稀释系统。APIMS对杂质检测的灵敏度与杂质的电离方式密切相关,电荷传递是杂质电离最主要的一种方式,适用于电离能相差较大的底气与杂质,常见的N₂、Ar由于电离能较高,其中的大部分杂质均可依靠该方式测定;质子转移反应的应用通常与H₂有关,常用于H₂中杂质的测定,也可以通过添加H₂的方法促进对Ar中N₂杂质的检测;运用形成团簇离子的反应尽管较少,但亦有报道,通过监测团簇离子O₂⁺·H₂O,可提高O₂中杂质H₂O的检测灵敏度。依据不同的电离反应,可以设计对不同杂质的测定方式,实现对痕量、超痕量杂质的检测。APIMS检测灵敏度通常比电子轰击电离质谱(EI/MS)高10⁴~10⁶倍,因此目前依然是超高纯气体分析中不可替代的仪器方法,但在某些方面如对有腐蚀性电子特气的分析,方法灵敏度有待提高。     

单极-偶极时间域激电测深在建筑场地地下岩溶勘查中的应用

灰岩区的溶蚀现象不仅会导致基岩面起伏很大,还会产生溶蚀带、溶洞、土洞等地质现象,严重影响到该地区工程建设。近年来,根据溶洞、土洞与其围岩电性的差异,使用电法勘探寻找溶洞、土洞取得了较好的效果。单极-偶极时间域激电测深方法在建筑场地岩溶勘查中的应用表明,该方法对于查明建筑场地岩溶、土洞的存在以及分布范围是一种有效的地球物理勘探方法。     

Atmospheric Deposition Connected with Marine Primary Production,Nitrogen Cycle: A Review

Atmospheric Deposition (AD) provides external nutrients such as nitrogen (N), phosphorus (P) and iron (Fe) supporting the growth of phytoplankton in oceans and thereby exerts obvious impacts on carbon and nitrogen cycles and climate change associated. Specifically, the external nutrients derived from atmospheric deposition can promote the marine primary production and nitrogen fixation that enhance the ocean capacity in absorbing CO₂; AD may also change a few pathways of carbon and nitrogen cycles in oceans and increase the emissions of biogenic aerosol and radioactive gases such as N₂O, DMS, etc. Due to the underlying important impacts on climate and environmental change, AD and processes related have become the hot topics of multidisciplinary studies in the areas of ocean and atmospheric sciences, and the focus of some international core projects such as Surface Ocean Lower Atmosphere Study (SOLAS), an International Study of Marine Biogeochemical Cycles of Trace Elements and Their Isotopes (GEOTRACES) and Integrated Marine Biogeochemistry and Ecosystem Research (IMBER). With the severe air pollution and high frequencies of Asian dust events, as the downwind areas of big cities and dust sources, the East China Sea and adjacent North Pacific have received increasing influences of AD. Limited studies showed that the increase of AD indeed caused significant influence on carbon and nitrogen cycles in these immediately related oceanic areas and the study there would have a signature effect on global oceans. A multidisciplinary study on the impacts of AD in oceans, e.g., combing molecular biology and experimental ecology techniques to study primary production processes, utilizing isotopic techniques to trace the change of the nitrogen cycle, new evidences of ocean-biogenic aerosol emissions, etc. would be the focus in the future.     

Depth profiles of volatile iodine and bromine-containing halocarbons in coastal Antarctic waters

Measurements of bromoform (CHBr₃), diiodomethane (CH₂I₂), chloroiodomethane (CH₂ICl) and bromoiodomethane (CH₂IBr) were made in the water column (5–100 m depth) of the Southern Ocean within 0–40 km of the Antarctic sea ice during the ANTXX1/2 transect of the German R/V Polarstern, at five locations between 70–72°S and 9–11°W in the Antarctic spring/summer of 2003–2004. Some of the profiles exhibited a very pronounced layer of surface sea-ice meltwater, as evidenced by salinity minima and temperature maxima, along with surface maxima in concentrations of CHBr₃, CH₂I₂, CH₂ICl and CH₂IBr. These results are consistent with in situ surface halocarbon production by ice algae liberated from the sea ice, although production within the sea ice followed by transport cannot be entirely ruled out. Additional sub-surface maxima in halocarbons occurred between 20 and 80 m. At a station further from shore and not affected by surface sea-ice meltwater, surface concentrations of CH₂I₂ were decreased whereas CH₂ICl concentrations were increased compared to the stations influenced by meltwater, consistent with photochemical conversion of CH₂I₂ to CH₂ICl, perhaps during upward mixing from a layer at  70 m enhanced in iodocarbons. Mean surface (5–10 m) water concentrations of halocarbons in these coastal Antarctic waters were 57 pmol l^− 1 CHBr₃ (range 44–78 pmol l^− 1), 4.2 pmol l^− 1 CH₂I₂ (range 1.7–8.2 pmol l^− 1), 0.8 pmol l^− 1 CH₂IBr (range 0.2–1.4 pmol l^− 1), and 0.7 pmol l^− 1 CH₂ICl (range 0.2–2.4 pmol l^− 1). Concurrent measurements in air suggested a sea-air flux of bromoform near the Antarctic coast of between 1 and 100 (mean 32.3, median 10.4) nmol m^− 2 day^− 1 and saturation anomalies of 557–1082% (mean 783%, median 733%), similar in magnitude to global shelf values. In surface samples affected by meltwater, CH₂I₂ fluxes ranged from 0.02 to 6.1 nmol m^− 2 day^− 1, with mean and median values of 1.9 and 1.1 nmol m^− 2 day^− 1, respectively.     

Transterminator ion flow in the Martian ionosphere

The upper ionospheres of Mars and Venus are permeated by the magnetic fields induced by the solar wind. It is a long-standing question whether these fields can put the dense ionospheric plasma into motion. If so, the transterminator flow of the upper ionosphere could explain a significant part of the ion escape from the planets atmospheres. But it has been technically very challenging to measure the ion flow at energies below 20 eV. The only such measurements have been made by the ORPA instrument of the Pioneer Venus Orbiter reporting speeds of 1-5 km/s for O⁺ ions at Venus above 300 km altitude at the terminator ( [Knudsen et al., 1980] and [Knudsen et al., 1982]). At Venus the transterminator flow is sufficient to sustain a permanent nightside ionosphere, at Mars a nightside ionosphere is observed only sporadically. We here report on new measurements of the transterminator ion flow at Mars by the ASPERA-3 experiment on board Mars Express with support from the MARSIS radar experiment for some orbits with fortunate observation geometry. We observe a transterminator flow of O⁺ and O₂⁺ ions with a super-sonic velocity of around 5 km/s and fluxes of 0.8×10⁹/cm² s. If we assume a symmetric flux around the terminator this corresponds to an ion flow of 3.1±0.5×10²⁵/s half of which is expected to escape from the planet. This escape flux is significantly higher than previously observed on the tailside of Mars. A possible mechanism to generate this flux can be the ionospheric pressure gradient between dayside and nightside or momentum transfer from the solar wind via the induced magnetic field since the flow velocity is in the Alfvénic regime. We discuss the implication of these new observations for ion escape and possible extensions of the analysis to dayside observations which may allow us to infer the flow structure imposed by the induced magnetic field.     

On the maintenance of thermal wind balance and equatorial superrotation in Titan's stratosphere

Titan's atmospheric winds, like those on Venus, exhibit superrotation at high altitudes. Titan general circulation models have yielded conflicting results on whether prograde winds in excess of 100 m s⁻¹ at the 1 mbar level are possible based on known physical processes that drive wind systems. A comprehensive two-dimensional (2D) model for Titan's stratosphere was constructed to systematically explore the physical mechanisms that produce and maintain stratospheric wind systems. To ensure conservation of angular momentum in the limit of no net exchange of atmospheric angular momentum with the solid satellite and no external sources and sinks, the zonal momentum equation was solved in flux form for total angular momentum. The relationships among thermal wind balance, meridional circulation, and zonal wind were examined with numerical experiments over a range of values for fundamental input parameters, including planetary rotation rate, radius, internal friction due to wave stresses, and net radiative drive. The magnitude of mid-latitude jets is most sensitive to a single parameter, the planetary rotation rate and results from the conversion of planetary angular momentum to relative angular momentum by the meridional circulation, whereas the strength of meridional circulation is mainly determined by the magnitude of the radiative drive. For Titan's slowly rotating atmosphere, the meridional temperature gradient is vanishingly small, even when the radiative drive is enhanced beyond reasonable magnitudes, and can be inferred from zonal winds in gradient/thermal wind balance. In our 2D model large equatorial superrotation in Titan's stratosphere can be only produced through internal drag forcing by eddy momentum fluxes, which redistribute angular momentum within the atmosphere, while still conserving the total angular momentum of the atmosphere with time. We cannot identify any waves, such as gravitational or thermal tides, that are sufficiently capable of generating the required eddy forcing of >50 m s⁻¹ Titan-day⁻¹ to maintain peak prograde winds in excess of 100 m s⁻¹ at the 1 mbar level.