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   

环境植物样品中铜铅锌铁锰的测定     

马欣  丛玉梅  邵文君 《国土资源》1995,(1)

将环境植物样品在４００─５００℃灰化，用硝酸、氢氟酸和高氯酸分解，用盐酸（１＋１）提取，控制２％─３％的盐酸介质，用火焰原子吸收分光光度法测定环境植物样品中的微量铜、铅、锌、铁、锰。该方法简单、快速、可靠。对环境植物标准样品的测定结果理想。  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   

Rotationally-resolved spectroscopy of Vesta I: 2-4 μm region     

A.S. Rivkin  L.A. McFadden  M. Sykes 《Icarus》2006,180(2):464-472

We present new infrared (2-4 μm) spectroscopic observations of Vesta obtained in 2001, 2003, and 2004. Together with previously published work, these present a picture of how Vesta's spectrum changes with sub-Earth latitude and longitude. Vesta's albedo and 2-μm band vary regularly with its rotational phase. While establishing the continuum level for Vesta in the 3-μm region is not straightforward, Vesta appears to have a spectrum consistent with the HED meteorites and not requiring a 3-μm water of hydration band. We cannot formally rule out a shallow (∼1%) band, however. We place limits on the extent to which solar-wind implantation and contamination by CM-like impactors has changed the surface spectrum of Vesta.  相似文献   

Latitudinal variations of CO and OCS in the lower atmosphere of Venus from near-infrared nightside spectro-imaging     

Emmanuel Marcq  Bruno Bézard  Mirel Birlan 《Icarus》2005,179(2):375-386

Spectro-imaging of Venus' nightside in the 2.3-μm window provides a powerful means of probing the lower atmosphere in the 25-40 km altitude range. We present observations recorded at the NASA/IRTF in February 2003 and August 2004, using the SpeX spectro-imager in the 2.1-2.5-μm region. Abundances of CO and OCS have been derived as a function of latitude for different longitudes. The CO abundance increases by about 15% between the equatorial region and higher latitudes (±40°). No longitudinal or temporal variations are observed. The OCS abundance shows the opposite variation in observational sets with sufficient S/N. These variations and anticorrelation are consistent with upwelling motions in the equatorial region and downwelling at higher latitudes.  相似文献   

E5000型全谱直读型电弧发射光谱仪研制及其在地球化学样品分析中应用   总被引：2，自引：2，他引：0  

俞晓峰  李锐  寿淼钧  郑存江  胡勇平 《岩矿测试》2015,34(1):40-47

在地球化学样品检测工作中,Ag、B、Sn等难分析元素通常采用传统的交流电弧发射光谱法(摄谱仪),随着地球化学样品数量的增加以及对检测结果质量要求的提高,该方法操作复杂、分析过程繁琐的问题与日常大量样品分析的矛盾日益突出,多道式电弧直读发射光谱也开始在行业内应用。本文基于先进的数字光源技术和CCD全谱型光谱仪技术,改进了电弧发生系统、分光系统和检测系统,将电弧激发光源与Paschen-Runge型全谱CCD光谱仪结合,研制了一款新型的台式全谱直读型电弧发射光谱仪E5000。E5000型电弧发射光谱仪通过激光定位结合程控电极技术,自动调整电极位置,提高了采谱过程的精度控制;利用CCD全谱技术获得了激发样品的全谱信息,可轻易实现光谱信号的背景扣除和干扰校正;且无需再次测定黑度,直接获得分析结果;同时结合内标法和标准加入法,可以进一步提高复杂基体样品的分析精准度。应用研制的光谱仪对水系沉积物和土壤样品进行检测,Ag、B、Sn元素的检出限分别达到了0.01μg/g、0.65μg/g、0.16μg/g,在分析水系沉积物、土壤时检测精密度基本小于10%,优于当前的摄谱法和多道电弧直读光谱法,满足了地球化学样品检测质量要求。  相似文献   

电感耦合等离子体发射光谱法测定铅锌矿中15个主次量元素   总被引：3，自引：2，他引：1  

孟时贤  邓飞跃  杨远  苏卫汉  闵晓芳  雍伏曾 《岩矿测试》2015,34(1):48-54

铅锌矿多元素同时测定中,样品预处理过程受多种不同因素的影响,单因素试验往往无法同时为多因素实验提供合理的优化方案。本文采用盐酸-硝酸溶矿,考察了样品预处理过程中混合酸配比、混合酸体积、消解时间及消解温度对消解效果的影响,利用正交试验设计及极差分析确定了最优消解条件:盐酸-硝酸混合酸配比3∶1,混合酸体积10 m L,消解时间120 min,消解温度90℃,用电感耦合等离子体发射光谱法同时测定铅锌矿中15个主次量元素(铅锌铜锰砷银铋镉钴镍镓铟钼锗锑)的含量。在最优条件下,用富铅锌矿石国家标准物质(GBW 07165)进行试验,大多数元素的精密度(RSD,n=12)和准确度小于5%,方法检出限为0.0019~0.048μg/g。基于铅锌矿主要是以硫化物形式存在,采用一系列硫化物国家标准物质验证方法的准确度及可行性,检测结果基本都在标准值的误差范围内。应用该方法分析湖南某矿区中大批量铅锌矿样品,标样质量统计合格率为100%,密码质量统计合格率大于97%。  相似文献   

电感耦合等离子体发射光谱法测定硼硅酸盐玻璃中的硼等常见元素   总被引：2，自引：1，他引：1  

郭中宝  张艳妮  代铮  王潇 《岩矿测试》2015,34(1):55-59

硼硅酸盐玻璃中的硼、钙、镁、铝、铁、钛、硅等常见元素普遍采用各元素分别测定的方式进行分析,分析效率很低;而且硼的测定普遍采用容量法,当B2O3含量低于1%时,容量法测定误差较大。本文以KOH熔融的方式消解样品,采用电感耦合等离子体发射光谱法(ICP-AES)进行分析。通过实验研究了KOH用量和不同称样量对B2O3测定结果的影响。结果表明,KOH用量在3 g以上时有较好的熔样效率和熔样效果,称样量低于0.4 g对B2O3测定结果无明显影响,考虑到其他元素的测定,确定了KOH用量优选3 g,称样量优选0.1 g。在此条件下,测定B2O3等常见元素的精密度(RSD,n=6)≤2%,加标回收率在96.0%~105.6%之间,除Si O2测定误差较大外,其他元素的测定结果均令人满意。本方法确定的B2O3的定量限为0.067%,且对于B2O3最高含量达到16%的测定结果也令人满意,因此可测定B2O3含量的范围至少为0.067%~16%。当样品中的B2O3含量高于4%时,方法准确度和精密度与国家标准分析方法(容量法)相当;当B2O3含量低于1%时,方法准确度和精密度都优于容量法。与现有报道相比,本方法显著拓宽了B2O3的测定范围,并具有良好的准确度,而且在B2O3准确测定的同时,也实现了Ca、Mg、Al、Fe、Ti的定量分析和Si的半定量分析,大大提高了分析效率,可以实现硼硅酸盐玻璃中B2O3等常见元素的准确快速分析。  相似文献