Titan trace gaseous composition from CIRS at the end of the Cassini-Huygens prime mission     

A. Coustenis  D.E. Jennings  R.K. Achterberg  S. Vinatier  N.A. Teanby  R.C. Carlson  G. Bampasidis  P.N. Romani 《Icarus》2010,207(1):461-18

This paper reports on the results from an extensive study of all nadir-looking spectra acquired by Cassini/CIRS during the 44 flybys performed in the course of the nominal mission (2004-2008). With respect to the previous study (Coustenis, A., and 24 colleagues [2007]. Icarus 189, 35-62, on flybys TB-T10) we present here a significantly richer dataset with, in particular, more data at high northern and southern latitudes so that the abundances inferred here at these regions are more reliable. Our enhanced high-resolution dataset allows us to infer more precisely the chemical composition of Titan all over the disk. We also include improved spectroscopic data for some molecules and updated temperature profiles. The latitudinal distributions of all of the gaseous species are inferred. We furthermore test vertical distributions essentially for acetylene (C₂H₂) from CIRS limb-inferred data and from current General Circulation Models for Titan and compare our results on all the gaseous abundances with predictions from 1-D photochemical-radiative models to check the reliability of the chemical reactions and pathways.  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   

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   

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   

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   

Optical spectroscopy of the radio pulsar PSR B0656+14     

S. Zharikov  R. E. Mennickent  Yu. Shibanov  V. Komarova 《Astrophysics and Space Science》2007,308(1-4):545-549

We have obtained the spectrum of a middle-aged PSR B0656+14 in the 4300–9000 Å range with the ESO/VLT/FORS2. Preliminary results show that at 4600–7000 Å the spectrum is almost featureless and flat with a spectral index α _ν ??0.2 that undergoes a change to a positive value at longer wavelengths. Combining with available multiwavelength data suggests two wide, red and blue, flux depressions whose frequency ratio is about 2 and which could be the 1st and 2nd harmonics of electron/positron cyclotron absorption formed at magnetic fields ～10⁸ G in upper magnetosphere of the pulsar.  相似文献   

The organic composition of C/2001 A2 (LINEAR): II. Search for heterogeneity within a comet nucleus     

Erika L. Gibb  Michael A. DiSanti  Neil Dello Russo  Michael J. Mumma 《Icarus》2007,188(1):224-232

The nucleus of Comet C/2001 A2 (LINEAR) split several times during its recent apparition, presenting an unusual opportunity to search for chemical differences in freshly exposed material. We conducted this search using NIRSPEC at the W.M. Keck Observatory on four dates in 2001: 9.5 and 10.5 July and 4.4 and 10.5 August. We detected the R0 and R1 lines of the ν₃ vibrational band of CH₄ near 3.3 μm on all dates. The R2 line was detected on 4.4 and 10.5 August. When we compare production rates of CH₄ to H₂O, we find evidence of a significant enhancement in August relative to that found in July. H₂CO was securely detected via its ν₁ and ν₅ bands on 9.5 July. On 10.5 July, H₂CO emission was much weaker, and its mixing ratio had dropped by a factor of about four. The mixing ratios for other detected volatile species did not change significantly over the course of the observations. We discuss the implications of this evidence for chemical heterogeneity in the nucleus of Comet C/2001 A2.  相似文献   

Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign     

C.M. Lisse  K. Dennerl  S.J. Wolk  T.H. Zurbuchen  R. Hoekstra  C.D. Fry  T. Mäkinen 《Icarus》2007,190(2):391-405

We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ∼295 ks between 30th June and 24th July 2005, and continuously for ∼64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329-1347] was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in X-ray flux due to the Deep Impact event was small, ∼20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×¹⁰⁶ kg (∼10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, much stronger than the man-made increase due to Deep Impact, were found in the observed X-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma, with intermittent impulsive events due to solar flares and coronal mass ejections.  相似文献   

Ground-based near infrared spectroscopy of Jupiter's ring and moons     

Michael H. Wong  Imke de Pater 《Icarus》2006,185(2):403-415

The backscattered reflectivity of Jupiter's ring has been previously measured over distinct visible and near infrared wavelength bands by a number of ground-based and spaceborne instruments. We present spectra of Jupiter's main ring from 2.21-2.46 μm taken with the NIRSPEC spectrometer at the W.M. Keck observatory. At these wavelengths, scattered light from Jupiter is minimal due to the strong absorption of methane in the planet's atmosphere. We find an overall flat spectral slope over this wavelength interval, except for a possible red slope shortward of 2.25 μm. We extended the spectral coverage of the ring to shorter wavelengths by adding a narrow-band image at 1.64 μm, and show results from 2.27-μm images over phase angles of 1.2°-11.0°. Our images at 1.64 and 2.27 μm reveal that the halo contribution is stronger at the shorter wavelength, possibly due to the redder spectrum of the ring parent bodies as compared with the halo dust component. We find no variation in main ring reflectivity over the 1.2°-11.0° phase angle range at 2.27 μm. We use adaptive optics imaging at the longer wavelength L′ band (3.4-4.1 μm) to determine a 2-σ upper limit of 22 m of vertically-integrated I/F. Our observing campaign also produced an L′ image of Callisto, showing a darker leading hemisphere, and a spectrum of Amalthea over the 2.2-2.5 and 2.85-3.03 μm ranges, showing deep 3-μm absorption.  相似文献   

Spectral alteration of the Meteorite Epinal (H5) induced by heavy ion irradiation: a simulation of space weathering effects on near-Earth asteroids     

G. Strazzulla  E. Dotto  R. Brunetto  A. Blanco 《Icarus》2005,174(1):31-35

We present results obtained for Epinal (H5), an ordinary chondrite meteorite, irradiated with 60 keV Ar⁺⁺ ions, simulating solar wind heavy particle irradiation. Bidirectional reflectance spectra (0.3-2.67 μm) measured after irradiating Epinal samples with different ion fluences exhibit a progressive reddening that is similar to the spread of spectra observed for S-type near-Earth asteroids. The timescales for inducing the same effects in space as those obtained in laboratory are estimated to be ¹⁰⁴-¹⁰⁶ yr. These results suggest irradiation by heavy ions may be a very efficient weathering process in near-Earth space.  相似文献