Abundances of Jupiter's trace hydrocarbons from Voyager and Cassini     

C.A. Nixon  R.K. Achterberg  P.N. Romani  X. Zhang  P.G.J. Irwin 《Planetary and Space Science》2010,58(13):1667-1680

The flybys of Jupiter by the Voyager spacecraft in 1979, and over two decades later by Cassini in 2000, have provided us with unique datasets from two different epochs, allowing the investigation of seasonal change in the atmosphere. In this paper we model zonal averages of thermal infrared spectra from the two instruments, Voyager 1 IRIS and Cassini CIRS, to retrieve the vertical and meridional profiles of temperature, and the abundances of the two minor hydrocarbons, acetylene (C₂H₂) and ethane (C₂H₆). The spatial variation of these gases is controlled by both chemistry and dynamics, and therefore their observed distribution gives us an insight into both processes. We find that the two gases paint quite different pictures of seasonal change. Whilst the 2-D cross-section of C₂H₆ abundance is slightly increased and more symmetric in 2000 (northern summer solstice) compared to 1979 (northern fall equinox), the major trend of equator to pole increase remains. For C₂H₂ on the other hand, the Voyager epoch exhibits almost no latitudinal variation, whilst the Cassini era shows a marked decrease polewards in both hemispheres. At the present time, these experimental findings are in advance of interpretation, as there are no published models of 2-D Jovian seasonal chemical variation available for comparison.  相似文献   

Oxygen and carbon isotope ratios in the martian atmosphere     

Vladimir A. Krasnopolsky  Jean Pierre Maillard  Tobias C. Owen  Robert A. Toth  Michael D. Smith 《Icarus》2007,192(2):396-403

Oxygen and carbon isotope ratios in the martian CO₂ are key values to study evolution of volatiles on Mars. The major problems in spectroscopic determinations of these ratios on Mars are uncertainties associated with: (1) equivalent widths of the observed absorption lines, (2) line strengths in spectroscopic databases, and (3) thermal structure of the martian atmosphere during the observation. We have made special efforts to reduce all these uncertainties. We observed Mars using the Fourier Transform Spectrometer at the Canada–France–Hawaii Telescope. While the oxygen and carbon isotope ratios on Mars were byproducts in the previous observations, our observation was specifically aimed at these isotope ratios. We covered a range of 6022 to 6308 cm⁻¹ with the highest resolving power of ν/δν=3.5×10⁵ and a signal-to-noise ratio of 180 in the middle of the spectrum. The chosen spectral range involves 475 lines of the main isotope, 184 lines of ¹³CO₂, 181 lines of CO¹⁸O, and 119 lines of CO¹⁷O. (Lines with strengths exceeding 10⁻²⁷ cm at 218 K are considered here.) Due to the high spectral resolution, most of the lines are not blended. Uncertainties of retrieved isotope abundances are in inverse proportion to resolving power, signal-to-noise ratio, and square root of the number of lines. Laboratory studies of the CO₂ isotope spectra in the range of our observation achieved an accuracy of 1% in the line strengths. Detailed observations of temperature profiles using MGS/TES and data on temperature variations with local time from two GCMs are used to simulate each absorption line at various heights in each part of the instrument field of view and then sum up the results. Thermal radiation of Mars' surface and atmosphere is negligible in the chosen spectral range, and this reduces errors associated with uncertainties in the thermal structure on Mars. Using a combination of all these factors, the highest accuracy has been achieved in measuring the CO₂ isotope ratios: ¹³C/¹²C = 0.978 ± 0.020 and ¹⁸O/¹⁶O = 1.018 ± 0.018 times the terrestrial standards. Heavy isotopes in the atmosphere are enriched by nonthermal escape and sputtering, and depleted by fractionation with solid-phase reservoirs. The retrieved ratios show that isotope fractionation between CO₂ and oxygen and carbon reservoirs in the solid phase is almost balanced by nonthermal escape and sputtering of O and C from Mars.  相似文献   

Gemini-N mid-IR observations of the dust properties of the ejecta excavated from Comet 9P/Tempel 1 during Deep Impact     

David E. Harker  Charles E. Woodward  R. Scott Fisher 《Icarus》2007,190(2):432-453

We present mid-infrared spectra and images from the Gemini-N (+MICHELLE) observational campaign of Comet 9P/Tempel 1 before, during, and after its encounter with Deep Impact. We use our thermal grain model to probe the 10 μm properties of the dust grains in the coma of the comet. Before impact (3 July 2005 UT), and more than 24 h after impact (5, 16, and 28 July 2005 UT), the comet dust grains were composed mostly of amorphous olivine, and were relatively large (peak of the grain size distribution ). For the night of impact, we extract spectra by centering on the nucleus, and offset 1″ from the nucleus in the direction of the impact ejecta plume. We find small dust grains (∼0.2 μm) of a diverse mineralogy (amorphous olivine, amorphous pyroxene, amorphous carbon, and crystalline olivine) populating the ejecta. The submicron sized dust grains move faster than the other, larger grains (?0.7 μm), with amorphous olivine and amorphous carbon traveling together, and amorphous pyroxene and crystalline olivine dispersing at a similar rate. Deriving a velocity law from a time-of-flight analysis, we find that the material traveled with a velocity law scaled by and with a power of p=0.5. This velocity power-law requires a sustained release of grains for the duration of 45-60 min after impact. Since the mineral species are traveling at different speeds, and there was a sustained release of grains due to a possible “gas-plume,” we conclude that the different minerals did not originate from grain aggregates destroyed by the impact, but instead arise from an inhomogeneous nucleus.  相似文献   

Integration of intensity textures and local geometry descriptors from Terrestrial Laser Scanning to map chert in outcrops     

《ISPRS Journal of Photogrammetry and Remote Sensing》2014

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直流电弧原子发射光谱法测定钛和钛合金中微量杂质元素     

王辉  马晓敏  郑伟  王宽 《岩矿测试》2014,33(4):506-511

高纯度的钛及钛合金具有良好的可塑性,当有杂质存在时变得脆而硬而影响其性能,准确分析杂质元素的含量有利于对钛生产工艺进行质量控制。对于杂质元素的分析,现行国家标准方法是采用样品蒸发温度较高的直流电弧作为光源,摄谱仪测定,需要经过显影、定影、测量黑度等步骤,操作繁琐,流程长,测量误差较大。本文应用中阶梯光栅和电荷耦合器件(CCD)组成的直流电弧(DC Arc)原子发射光谱仪(波长范围200~800nm),谱线干扰分析和谱线强度测量可以同时进行,能更大限度地获取光谱信息,建立了快速测定钛及钛合金中10种微量杂质元素(锰锡铬镍铝钼钒铜锆钇)的分析方法。实验讨论了测定过程中的四类谱线干扰,包括钛作为基体元素的谱线干扰、钛合金中添加的化学成分元素干扰、铁谱线的干扰、杂质元素之间的干扰,确定了适当的分析线;并应用一种浅孔薄壁细颈杯形电极装入试样,提高了样品的蒸发效果;用氯化银和碳粉的混合物作缓冲剂,提高了待测元素的谱线强度。本方法的检测范围为0.001%~0.06%,精密度小于15%,回收率为90.0%~110.0%,适合于大批量钛及钛合金样品中杂质元素的同时检测。  相似文献   

壳聚糖和PDMDAAC改性膨润土用于处理含油废水的研究   总被引：1，自引：0，他引：1  

邵红  刘相龙  王大卫  徐微雪 《岩矿测试》2014,33(3):426-432

含油废水污染范围广,对人类和生态环境危害大。采用常规方法(如浮选法、絮凝法、电化学法、膜分离法和生物法)处理的除油率不高于91%,成本较高,因此急需开发一种高效低廉的吸附剂。膨润土是一种优良的吸附剂,但用其直接处理含油废水的效果较低。本文选用壳聚糖和PDMDAAC两种有机物作为改性剂,对钠基膨润土改性,使膨润土能有效地处理含油废水。通过实验比较了两种有机改性膨润土处理含油废水的最佳去除条件,探讨了表征对其吸附性能的影响。去油效果结果表明:壳聚糖改性膨润土的除油率可达87.8%,PDMDAAC改性膨润土的除油率可达89.3%,处理所需时间少于15 min;除油效率和处理时间都优于常规方法。吸附性能表征结果显示,两种改性剂均以负载的方式和钠基膨润土颗粒结合,吸附性能良好;相比而言,PDMDAAC改性膨润土的处理效果比壳聚糖改性膨润土更好。PDMDAAC应用于含油废水的处理,具有成本低、效率高、操作简单的特点,在含油废水处理领域具有较好的应用前景。  相似文献   

红外光谱/扫描电镜等现代大型仪器岩石矿物鉴定技术及其应用   总被引：4，自引：3，他引：1  

杜谷  王坤阳  冉敬  王风玉  潘忠习 《岩矿测试》2014,33(5):625-633

传统的光学显微镜由于分辨率、放大倍数的限制,对于细微颗粒的定性分析不准确,矿物的定量分析存在一定的误差,对纳米-微米级矿物形貌及结构特征的观察束手无策。随着油气勘探及地质找矿的不断深入,需要提供岩石中所有矿物、孔隙及微量元素的信息,因此整合傅里叶红外光谱仪、X射线衍射仪、拉曼光谱仪、扫描电镜的优点,建立以大型仪器为基础的岩石矿物鉴定方法是当前地质工作的需要。红外光谱光谱范围为7500~370 cm-1,能对固、液、气样品中含量高于30%的矿物进行快速、准确的定性分析;主要用于有机质分析,其次还可对部分具有极性键的无机化合物及金属氧化物进行分析。X射线衍射仪能快速地对样品中含量大于15%的矿物进行较为准确的定量分析;现今主要用于各类晶质矿物的定性分析,同时也可对碳酸盐岩矿物等不含水矿物进行定量分析。拉曼光谱仪光谱范围为200~1000 nm,空间分辨率为横向0.5μm、纵向2μm,通过对包裹体进行测试能直接获得成岩过程中的温度、压力、流体成分等信息;目前主要用于流体包裹体成分的测试,其次还可对分子极化度会发生变化的液态、粉末及固体样品进行定性分析。扫描电镜分辨率达到1 nm,能清晰地观察到纳米-微米级矿物的形貌特征及矿物的结构特征;主要用于纳米-微米级的任何非磁性固体矿物的形貌及相关关系的观察。通过大型仪器建立的岩石矿物鉴定方法具有更高的分辨率,显著地提高了岩矿鉴定的精准度,大大拓宽了岩矿鉴定的范围(如鉴定纳米/微米级的矿物、矿物的不同变种等),能够全面、精准地提供岩石矿物的矿物含量和矿物组成、客观准确的成岩作用信息、清晰的矿物微观形貌及结构特征,而且仪器功能相互重叠,测试结果相互验证,保证了测试结果的可靠性。与传统光学显微镜鉴定方法相比,现代大型仪器岩石矿物鉴定技术为揭示矿物间的共生、反应、演化、岩石的成因、沉积/成岩环境等提供了依据,为地质工作提供准确、全面的矿物定性定量、组构特征及成岩作用等信息,为地质工作的顺利完成奠定了坚实的基础。  相似文献   

藏南沙拉岗锑矿流体包裹体红外显微测温研究   总被引：4，自引：0，他引：4  

孙晓明  莫儒伟  翟伟  韦慧晓  周峰  梁业恒  张相国  易建洲 《岩石学报》2014,30(1):189-198

沙拉岗锑矿是藏南金锑成矿带内最具有代表性的锑矿床。为了更直接地了解该矿床的流体物理化学特征,本文利用红外显微镜对辉锑矿及紧密共生石英中的流体包裹体进行了显微测温研究。红外显微测温分析结果表明,辉锑矿中包裹体均一温度在134.9～221.9℃,峰值在160～190℃之间,盐度在1.7%～7.3%NaCleqv,峰值在5.0%～6.0%NaCleqv之间,密度在0.879～0.958g/cm3之间,平均值为0.934g/cm3;共生石英中包裹体均一温度在142.5～205.6℃,峰值在160～190℃之间,盐度在2.3%～7.0%NaCleqv,峰值在4.0%～6.0%NaCleqv之间,密度在0.910～0.947g/cm3之间,平均值为0.929g/cm3。通过对比研究认为沙拉岗辉锑矿及共生石英形成于同一物理化学条件,捕获同一成矿流体。结合石英中单个流体包裹体激光拉曼成分分析认为成矿流体为含微量CO2、N2、CH4气体的低温、低盐度和低密度的NaCl-H2O热液体系。成矿流体的沸腾作用是辉锑矿大量沉淀主要原因。  相似文献   

NH₄Cl水溶液的微观结构和宏观物性研究          下载免费PDF全文

张宇  李非  费莉婷  纪志永  赵颖颖  郭小甫  刘杰  王士钊  汪婧  毕京涛  张盼盼  张丁予  袁俊生 《盐湖研究》2022,30(4)

通过拉曼光谱、同步辐射X射线散射和密度泛函理论(DFT)模拟,研究了质量分数为1.0 %-28.0 %的NH₄Cl水溶液的微观结构变化。同时在室温下测量了粘度、接触角和电导率。由拉曼光谱和密度泛函理论模拟结果可知,当溶质浓度升高至10.0 %时,在2900 cm_-1^和3100 cm_-1^{附近出现了明显的}N-H作用峰,且随着质量分数的升高,NH₄Cl水溶液中的氢键类型发生了转变。X射线散射结果表明,当NH₄Cl水溶液质量分数升高至10.0 %时,差值对分布函数G(r)在2.98 ?附近出现明显双峰,表明在该浓度下溶液中NH₄₊^-Cl_-^{接触离子对开始成为主要微观作用形式。对}NH₄Cl水溶液的宏观物性研究表明,粘度、接触角和电导率均随着NH₄Cl水溶液质量分数的增加而增大。作者推断,NH₄Cl水溶液中氢键类型的转变、O-H...N键占比增多以及逐渐增加的NH₄₊^-Cl_-^{接触离子对},是粘度和接触角随溶质浓度增加而增加的微观本质因素;电导率的增加与溶液中有效导电离子数量增加有关。  相似文献   

红外波段太阳观测技术方法研究     

曹文达 《天文研究与技术》2002,(1)

1m红外太阳塔是我国未来重点发展的地面太阳观测设备 ,本文的所有工作均围绕着与此相关的红外波段太阳观测技术方法展开。1 .针对望远镜实验平台—云台太阳光谱仪 ,建立了光谱仪分光流量模型 ,并用多种实验手段验证了其可靠性。利用该模型计算了FeⅠ 1 .56μm红外太阳光谱的分光流量 ,分析了实验观测的可行性及改进方案。2 .针对探测器实验平台—PtSi红外焦平面阵列相机 ,建立了FeⅠ 1 .56μm光谱观测信噪比模型 ,模拟了各种噪声对观测的影响。在此基础上 ,在国内首次成功进行了FeⅠ1 .56μm红外太阳光谱的面阵观测实验。3 .在红外观测实验所处的高背景低对比度条件下 ,讨论了红外太阳光谱观测的图像处理方法 ,分析了观测中出现的干涉条纹的来源及解决办法 ,初步建立起了一整套红外太阳光谱与成像的定标方法和图像处理方法。4 .首次利用PVA材料 ,设计研制了一套FeⅠ 1 .56μm近红外Stokes参量偏振仪 ,并将该偏振仪安装在美国国立天文台McMath望远镜上进行了观测实验。针对一太阳黑子 ,通过扫描进行了二维的Stokes参量观测。同时建立了一套从Stokes参量反演磁矢量场的方法 ,并将反演的结果与怀柔太阳磁场望远镜的观测结果进行了比对。5.针对 1m红外太阳塔的太阳光谱仪系统 ,给出了垂直多波段光谱仪和红外  相似文献