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1.
Silicon carbide (SiC) is a particularly interesting species of presolar grain because it is known to form on the order of a hundred different polytypes in the laboratory, and the formation of a particular polytype is sensitive to growth conditions. Astronomical evidence for the formation of SiC in expanding circumstellar atmospheres of asymptotic giant branch (AGB) carbon stars is provided by infrared (IR) studies. However, identification of the crystallographic structure of SiC from IR spectra is controversial. Since >95% of the presolar SiC isolated from meteorites formed around carbon stars, a determination of the structure of presolar SiC is, to first order, a direct determination of the structure of circumstellar SiC. We therefore determined the polytype distribution of presolar SiC from the Murchison CM2 carbonaceous meteorite using analytical and high-resolution transmission electron microscopy (TEM). High-resolution lattice images and electron diffraction of 508 individual SiC grains demonstrate that only two polytypes are present, the cubic 3C (β-SiC) polytype (79.4% of population by number) and the hexagonal 2H (α-SiC) polytype (2.7%). Intergrowths of these two polytypes are relatively abundant (17.1%). No other polytypes were found. A small population of one-dimensionally disordered SiC grains (0.9%), whose high density of stacking faults precluded classification as any polytype, was also observed. The presolar origin of 2H α-SiC is unambiguously established by tens-of-nanometers-resolution secondary ion mass spectroscopy (NanoSIMS). Isotopic maps of a TEM-characterized 2H α-SiC grain exhibit non-solar isotopic compositions of 12C/13C = 64 ± 4 and 14N/15N = 575 ± 24. These measurements are consistent with mainstream presolar SiC thought to originate in the expanding atmospheres of AGB carbon stars. Equilibrium condensation calculations together with inferred mineral condensation sequences predict relatively low SiC condensation temperatures in carbon stars. The laboratory observed condensation temperatures of 2H and 3C SiC are generally the lowest of all SiC polytypes and fall within the predictions of the equilibrium calculations. These points account for the occurrence of only 2H and 3C polytypes of SiC in circumstellar outflows. The 2H and 3C SiC polytypes presumably condense at different radii (i.e., temperatures) in the expanding stellar atmospheres of AGB carbon stars.  相似文献   

2.
采用X射线衍射技术(XRD)对水镁石原矿和不同工艺条件生产的出口镁砂产品进行了物相组成分析,水镁石原矿粉中主相Mg(OH)2含量达到85.9%,杂质主要是Mg3Si2(OH)4O5、CaCO3和CaMg(CO3)2;轻烧镁砂中的Mg(OH)2大部分已经分解为MgO,但还有12.3%的Mg(OH)2未分解,并在低温煅烧的情况下生成了微量的新相Mg2SiO4;重烧镁砂中的Mg(OH)2已经完全分解为MgO,杂质主要存在形式是Mg2SiO4和CaCO3,占总量的18.5%。实验结果将成为提高水镁石矿煅烧生产的镁砂品质而改进提纯工艺的参考依据。  相似文献   

3.
The phase and melting relations of the C-saturated C–Mg–Fe–Si–O system were investigated at high pressure and temperature to understand the role of carbon in the structure of the Earth, terrestrial planets, and carbon-enriched extraterrestrial planets. The phase relations were studied using two types of experiments at 4 GPa: analyses of recovered samples and in situ X-ray diffractions. Our experiments revealed that the composition of metallic iron melts changes from a C-rich composition with up to about 5 wt.% C under oxidizing conditions (ΔIW = ?1.7 to ?1.2, where ΔIW is the deviation of the oxygen fugacity (fO2) from an iron-wüstite (IW) buffer) to a C-depleted composition with 21 wt.% Si under reducing conditions (ΔIW < ?3.3) at 4 GPa and 1,873 K. SiC grains also coexisted with the Fe–Si melt under the most reducing conditions. The solubility of C in liquid Fe increased with increasing fO2, whereas the solubility of Si decreased with increasing fO2. The carbon-bearing phases were graphite, Fe3C, SiC, and Fe alloy melt (Fe–C or Fe–Si–C melts) under the redox conditions applied at 4 GPa, but carbonate was not observed under our experimental conditions. The phase relations observed in this study can be applicable to the Earth and other planets. In hypothetical reducing carbon planets (ΔIW < ?6.2), graphite/diamond and/or SiC exist in the mantle, whereas the core would be an Fe–Si alloy containing very small amount of C even in the carbon-enriched planets. The mutually exclusive nature of C and Si may be important also for considering the light elements of the Earth’s core.  相似文献   

4.
29Si NMR shieldings have been calculated by ab initio coupled Hartree-Fock perturbation theory for the orthosilicate species Si(OH)4, Si(OH)3O-, Si(OH)2O 2 2- , Si(OH)O 3 3- and SiO 4 4- using energy optimized geometries from ab initio Hartree-Fock calculations. The shielding of Si(OH)3O- is smaller than that of Si(OH)4 by 2.7 ppm and the shielding trend along the Si(OH)4 to SiO 4 4- series is decidedly nonlinear. The unprotonated O in Si(OH)3O- is more shielded and has a much smaller electric field gradient than do the protonated oxygens. Calculated anisotropies show the largest components of the shielding to lie along or near the short Si-O bonds. Calculations employing point charges in place of H reproduce the shielding trends in T d and S 4 symmetry Si(OH)4 semiquantitatively. The calculated trends in shielding with < si-o-h=" can=" also=" be=" correlated=" with=" the=" energies=" of=" the=" si3p,o2p="> bonding orbitals.  相似文献   

5.
We report the results of SIMS isotopic analyses of carbon, nitrogen, oxygen, and silicon made on 849 small (approximately 1 micrometer) individual silicon carbide grains from the Murchison meteorite. The isotopic compositions of the major elements carbon and silicon of most grains (mainstream) are similar to those observed in larger grain studies suggesting an AGB star origin of these grains. In contrast, the trace element nitrogen shows a clear dependency on grain size. 14N/15N ratios increase with decreasing grain size, suggesting different stellar sources for grains of different size. Typically observed 14N/15N ratios in the small grains of this study are approximately 2700, clearly larger than the values expected from model calculations of AGB stars. In addition to the three dredge-up episodes characteristic for the evolution of AGB stars, extra-mixing of CNO-processed matter in low mass AGB stars appears to be a promising possibility in order to explain the high 14N/15N ratios of the small circumstellar SiC grains. A small fraction of grains shows a silicon isotopic signature not observed in larger circumstellar SiC grains from Murchison. Their stellar origin is still uncertain. The minor type A, B, Y, and X grains were found to be present at a level of a percent, which is similar to their abundance in the larger-grain SiC separates from Murchison. Oxygen isotopic compositions are normal within the experimental uncertainties of several 10%, indicating that oxygen of stellar origin is rare or even absent in the SiC grains. We conclude that most of the oxygen is a contaminant which was introduced into the SiC grains after their formation, e.g., during sample processing in the laboratory. We identified a nitride grain, most likely Si3N4 with little carbon, with highly anomalous isotopic compositions (12C/13C = 157 +/- 33, 14N/15N = 18 +/- 1, delta 29 Si = -43 +/- 56%, delta 30 Si = -271 +/- 50%). The isotopic patterns of carbon, nitrogen, and silicon resemble those of the rare SiC X grains suggesting that these two rare constituents of circumstellar matter formed in the same type of stellar source, namely, Type II supernovae.  相似文献   

6.
刘羽 《矿物岩石》2000,20(2):1-4
本文用电子探针成分分析,Ｘ射线单晶结构分析,振动光谱等手段对意大利武图列火山地区碳酸岩－超碱性岩杂岩体中磷灰石的晶体化学特征进行了研究。结果表明：该磷灰石的晶体化学式为：（Ｃａ９．８１Ｓｒ０．０５Ｍｎ０．０１ＬＲＥＥ０．０４Ｎａ０．０９）「Ｐ５．５０Ｓｉ０．０１５Ｓ０．０５Ｃ０．３０」Ｏ２３．７（Ｆ０．８０Ｃｌ０．０３ＯＨ１．１７）,属氟羟磷灰石,其结构中在钙多面体与磷氧四面体位置上出现广泛的类质  相似文献   

7.
《Applied Geochemistry》2005,20(7):1357-1367
Cancrinite, sodalite, and zeolite A have been found to form upon contacting hyperalkaline simulated tank waste (STW) with vadose zone sediments from the Hanford Reservation. Here, soluble silica and STW are used to study mineral formation and transformation. Two Hanford sediment fractions (diameters <50 and >50 μm instead of soluble silica) are also used as silica sources for comparison. A series of batch experiments at 50 °C and 25 days duration were conducted by reacting 0.026 mol/kg soluble Si with 6 different STW solutions. The STW solutions differed in NaOH and Al concentrations. Cancrinite, sodalite, and zeolite A formed when soluble Si was used as the Si source. The minerals were characterized by X-ray diffraction (XRD), scanning electron microscopy (SEM), Fourier transform infrared spectroscopy (FT-IR), and 27Al and 29Si magic-angle spinning nuclear magnetic resonance (MAS-NMR). Larger NaOH and Al concentrations favored formation of the more compact structures of cancrinite and sodalite. At larger NaOH concentration more Al for Si substitution occurred in the tetrahedral sites. A greater Al(4)/Al(6) ratio in the solids was found for the higher Si/Al ratio solutions based on NMR results. Mixtures of cancrinite and sodalite were characterized by particles with lepispheric morphology. At low Al concentration, increasing NaOH resulted in distinct hexagonal, prismatic particles common to crystalline cancrinite. At low Al/Si ratio, the characteristic cubic morphology of zeolite was observed in addition to cancrinite and sodalite.  相似文献   

8.
Transmission Electron Microscopy (TEM) and High Resolution TEM (HRTEM) investigations were used to study a complex micro-structure of twin-related lamellae of 15R SiC polytype, in syntactic coalescence with 6H-SiC. The analysis of the local stacking microstructure by means of HRTEM revealed that the perfect structure of 15R polytype, (23)3 was locally interrupted by numerous adjoining stacking faults parallel to (0001) with stacking of the coupled (22) and (33) bilayers superimposed on the twin boundaries. HR images taken exactly across both the twin boundaries showed a zig-zag pattern (23) that switched to (32) by a twin coherent interfaces or, alternatively, a zig-zag pattern (32) which passed to (23) through an isolated (33), 6H like sequence. The selected area electron diffraction (SAED) patterns taken exactly above both the twin interfaces indicate classifying of the twin found in this study as a “Friedelian” reticular merohedric twinning. However, two indistinguishable twin operations matched the observed features: a reflection through rational plane (0001), and 180°-rotation around [0001]. Since individual Si and C atoms and even the SiC bilayer polarity could not be established from these HR images, the real twin law was deduced by taking into account that the coherent structural match at the interface could be guaranteed only by a 180°-rotation around [0001]. In order to explain the origin of the planar defects found in this sample, the growth mechanism and the influence of the low-energy stacking faults were considered.  相似文献   

9.
用XRD,SEM和TEM研究新型配合物Cu(C3N2H4)2(C4H5O4)2的超分子结构和微观形貌,并对新型晶体的平衡外形进行模拟计算,结果表明:该配合物分子具有丁二酸桥联的双核铜结构,中心铜离子处在2个咪唑和4个丁二酸以单齿配位组成的八面体中心,在ab平面,分子中有十四元大环,环内Cu(1)-Cu(2)原子间距为0.8031nm,C(2)-C(2′)为0.4183nm;在ac平面,沿着[010]方向分子内呈现凹的六边形纳米级孔洞;沿[100]方向分子依靠弱的氢键作用,层状堆积成三维超分子结构。此外,随着丁二酸的碳链沿[001]方向无限延伸,形成以铜离子为交叉中心的带状拓扑构型。SEM观察到晶体表面形成有明显的凹坑,区域呈现层状阶梯,说明晶体在(100)面遵照台阶-扭折模型呈层状生长结晶。TEM微区形貌像显示晶体存在条纹和缺陷结构,整体保持柱状构型,这与模拟的晶体平衡外形呈柱状一致。模拟结果表明晶体最易外显晶面为(100)面,外显比例达41.247%,这与晶体超分子层沿[100]方向通过氢键作用堆积,键作用力较弱密切相关。  相似文献   

10.
《Geochimica et cosmochimica acta》1999,63(19-20):3395-3406
Transmission electron microscopy (TEM), with energy dispersive X-ray (EDX) analysis and energy filtered transmission electron microscopy/electron energy loss spectroscopy (EFTEM/EELS), as well as powder X-ray diffraction (XRD) and scanning electron microscopy (SEM), have been used to study bed sediments from two acid mine drainage (AMD) sites in western Montana, USA. TEM and associated techniques, including sample preparation via epoxy impregnation and ultramicrotome sectioning, afford the opportunity to better interpret and understand complex water-rock interactions in these types of samples. For the sample taken from the first site (Mike Horse mine), ferrihydrite is the dominant phase, Si and Zn are the most abundant elements sorbed to ferrihydrite surfaces, and Pb is notably absent from ferrihydrite association. Three additional important metal-containing phases (gahnite, hydrohetaerolite, and plumbojarosite), that were not apparent in the powder XRD pattern because of their relatively low concentration, were identified in the TEM. The presence of these phases is important, because, for example, gahnite and plumbojarosite act as sinks for Zn and Pb, respectively. Therefore, the mobility of Pb from this part of the drainage system depends on the stability of plumbojarosite and the ability of ferrihydrite to sorb the released Pb. From thermodynamic data in the literature, we predict that Pb will be released by the dissolution of plumbojarosite above a pH of 4 to 5, but it will then be recaptured by ferrihydrite if the pH continues to rise to 5.5 and higher, irrespective of competition effects from other metals. Therefore, only a relatively narrow pH window exists in which Pb can escape this portion of the system as an aqueous species. For the sample taken from the other site included in this study (the Carbonate mine), jarosite and quartz are the dominant phases. Interestingly, however, the jarosites are both Pb-poor and Pb-enriched. In addition, TEM reveals the presence of microcrystalline hematite with Si, S, and P sorbed to its surfaces, a nearly pure amorphous Si, Al oxyhydroxide, and an amorphous silica phase containing minor amounts of Al, Ca, and Fe. Pb will probably be released from these mixed K-Pb jarosites above pH 4 to 5, but the Pb may be retarded by the strongly adsorbing microcrystalline hematite in this pH range. The sink for Al in this system is the amorphous Si, Al oxyhydroxide, not Al(OH)3 which is typically used in AMD modeling schemes.  相似文献   

11.
Pure titanate nanotubes and titanate nanotubes doped with iron (III) and chromium (III) were fabricated by the hydrothermal treatment in methanol and sodium hydroxide mixture. The fabricated nano tubes have high surface area, high aspect ratio, consisted of very good surface morphology and high metals dispersion. The morphology, crysralline phase, composition were characterized by powdered X-ray diffraction, scanning electron microscopy, transmission electron microscopy, Barrett-Joyner-Halenda methods and X-ray photoelectron spectroscopy. The results showed that nanotubes possess anatase phase and are composed up of 8–12 nm in diameter and 360–400 nm in length. The band gap of the titanium dioxide nanotubes was determined using transformed diffuse reflectance spectroscopy according to the Kubelka-Munk theory, showed pronounced band gap decrease on doped titanium dioxide nanotubes. The photocatalytic activity of doped nanotubes were evaluated in terms of degradation of phenol and photoreduction of carbon dioxide into methanol and ethanol under Ultra violet and Infra red irradiation. It was found that with iron (III) and chromium (III) doped titanium dioxide nanotubes exhibited much higher photocatalytic activity than undoped titanate nanotubes.  相似文献   

12.
We report isotopic ratio measurements of small SiC and Si3N4 grains, with special emphasis on presolar SiC grains of type Z, and new nucleosynthesis models for 26Al/27Al and the Ti isotopic ratios in asymptotic giant branch (AGB) stars. With the NanoSIMS we analyzed 310 SiC grains from Murchison (carbonaceous CM2 chondrite) separate KJB (diameters 0.25-0.45 μm) and 153 SiC grains from KJG (diameters 1.8-3.7 μm), 154 SiC and 23 Si3N4 grains from Indarch (enstatite EH4 chondrite) separate IH6 (diameters 0.25-0.65 μm) for their C and N isotopic compositions, 549 SiC and 142 Si3N4 grains from IH6 for their C and Si isotopic compositions, 13 SiC grains from Murchison and 66 from Indarch for their Al-Mg compositions, and eight SiC grains from Murchison and 10 from Indarch for their Ti isotopic compositions. One of the original objectives of this effort was to compare isotopic analyses with the NanoSIMS with analyses previously obtained with the Cameca IMS 3f ion microprobe. Many of the Si3N4 grains from Indarch have isotopic anomalies but most of these apparently originate from adjacent SiC grains. Only one Si3N4 grain, with 13C and 14N excesses, has a likely AGB origin. The C, N, and Si isotopic data show that the percentage of SiC grains of type Y and Z increase with decreasing grain size (from ∼1% for grains >2 μm to ∼5-7% for grains of 0.5 μm), providing an opportunity for isotopic analyses in these rare grains. Our measurements expand the number of Al-Mg analyses on SiC Z grains from 4 to 23 and the number of Ti analyses on Z grains from 2 to 11. Inferred26Al/27Al ratios of Z grains are in the range found in mainstream and Y grains and do not exceed those predicted by models of AGB nucleosynthesis. Cool bottom processing (CBP) has been invoked to explain the low 12C/13C ratios of Z grains, but this process apparently does not lead to increased 26Al production in the parent stars of these grains. This finding is in contrast to presolar oxide grains where CBP is needed to explain their high 26Al/27Al ratios. The low 46,47,49Ti/48Ti ratios found in Z grains and their correlation with low 29Si/28Si ratios extend the trend seen in mainstream grains and confirm an origin in low-metallicity AGB stars. The relatively large excesses in 30Si and 50Ti in Z grains are predicted by our models to be the result of increased production of these isotopes by neutron-capture nucleosynthesis in low-metallicity AGB stars. However, the predicted excesses in 50Ti (and 49Ti) are much larger than those found. Even lowering the strength of the 13C pocket cannot solve this discrepancy in a consistent way.  相似文献   

13.
The volatilization kinetics of single crystal α-SiC, polycrystalline β-SiC, and SiO2 (cristobalite or glass) were determined in H2-CO2, CO-CO2, and H2-CO-CO2 gas mixtures at oxygen fugacities between 1 log unit above and 10 log units below the iron-wüstite (IW) buffer and temperatures in the range 1151 to 1501°C. Detailed sets of experiments on SiC were conducted at 2.8 and 6.0 log units below IW (IW-2.8 and IW-6.0) at a variety of temperatures, and at 1300°C at a variety of oxygen fugacities. Transmission electron microscopic and Rutherford backscattering spectroscopic characterization of run products shows that the surface of SiC exposed to IW-2.8 is characterized by a thin (<1 μm thick), continuous layer of cristobalite. SiC exposed to IW-6.0 lacks such a layer (or its thickness is <0.01 μm), although some SiO2 was found within pits and along incised grain boundaries.In H2-CO2 gas mixtures above ∼IW-3, the similarity of the SiC volatilization rate and of its dependence on temperature and fO2 to that for SiO2 suggests that SiC volatilization is controlled by volatilization of a SiO2 layer that forms on the surface of the SiC. With decreasing log fO2 from ∼IW-3 to ∼IW-6, the SiC volatilization rate is constant at constant temperature, whereas that for SiO2 increases. The independence of the SiC volatilization rate from the gas composition under these conditions suggests that the rate-controlling step is a solid-solid reaction at the internal SiC/SiO2 interface. For gas compositions more reducing than ∼IW-6, the SiC volatilization rate increases with decreasing fO2, with both bare SiC surfaces and perhaps silica residing in pits and along incised grain boundaries contributing to the overall reaction rate.If the volatilization mechanism and reaction rate in the solar nebula were the same as in our H2-CO2 experiments at IW-6.0, then estimated lifetimes of 1-μm-diameter presolar SiC grains range from several thousand years at ∼900°C, to ∼1 yr at 1100°C, ∼1 d at 1300°C, and ∼1 h at 1400°C. The corresponding lifetimes for 10-μm SiC grains would be an order of magnitude longer. If the supply of oxidants to surfaces of presolar SiC grains were rate limiting—for example, at T > 1100°C for Ptot= 10−6 atm and sticking coefficient = 0.01, then the calculated lifetimes would be about 10 yr for 10-μm-diameter grains, essentially independent of temperature. The results thus imply that presolar SiC grains would survive short heating events associated with formation of chondrules (minutes) and calcium-, aluminum-rich inclusions (days), but would have been destroyed by exposure to hot (≥900°C) nebular gases in less than several thousand years unless they were coated with minerals inert to reaction with a nebular gas.  相似文献   

14.
现代植物植硅体化学组成研究有利于揭示植硅体的化学组成与细胞形态、植物种类及植物生长环境之间的关系,认识植硅体形成机制、植物分类及生态意义。植硅体化学组成测试方法多种多样,主要涉及植硅体化学元素组成及Si、O和C元素同位素组成测定,研究表明植硅体主要含二氧化硅和水,封闭有少量的有机成分及多种矿质元素。在植硅体封闭有机成分存在形式,部分元素的形成、迁移等循环机理,稳定碳同位素组成、分布及其生态指示意义以及^14C测年研究等方面取得一定认识。植物种类、组织部位、细胞微环境以及植物生长的环境因子能够影响植硅体的化学组成。植硅体化学组成研究对植硅体形成机制及碳、硅等元素循环具有重要意义,植硅体部分化学元素、植硅体稳定同位素组成及^14C测年具有较好的古环境及考古研究潜力。现代植物植硅体化学组成及其与环境因子的关系,以及植硅体电子探针微区研究有待于进一步深入开展。  相似文献   

15.
吴伟端  潘兆橹 《矿物学报》2000,20(4):397-400
选用气流磨超音速气流作为机械力,对硅灰石、硬脂酸进行超细粉碎－表面改性。应用透射电子显微镜分析、观察硅石灰／硬脂酸复合粉体界面微观形貌及成分（Ｃａ、Ｓｉ、Ｃ）的变化规律。ＴＥＭ能谱分析结果表明：从硅灰石到硬脂酸,Ｃａ、Ｓｉ含量逐渐降低,Ｃ含量则逐渐升高。  相似文献   

16.
The pore-water geochemistry and mineralogy of tailings derived from a granitic tungsten deposit were characterized by collecting pore-water samples at discrete depth intervals throughout the tailings for the analysis of major and minor element concentrations. Mineralogical samples from the oxidation zone were analyzed by X-ray diffraction, scanning electron microscopy combined with energy dispersive X-ray spectroscopy (SEM/EDS), electron microprobe (EMP) combined with wavelength dispersive X-ray spectroscopy (WDS), and transmission electron microscopy (TEM). The oxidation of sulfide minerals in the near-surface tailings leads to a decrease in pore-water pH and elevated SO4, As, and metal concentrations. The unusual mineralogy of this deposit, compared with that of commonly studied base-metal and gold deposits, results in several unique geochemical characteristics. The dissolution of fluorite releases F into the pore water; the F forms strong complexes with Al and enhances the dissolution of aluminosilicate minerals within the oxidation zone. As a result, high Al concentrations (up to 151.7 mg/L) are detected in the near-neutral pore water in the oxidation zone. The combined dissolution of aluminosilicates and carbonate minerals maintains the pH near 10 in the pore water at depth. Elevated concentrations of W (up to 7.1 mg/L) are detected in the pore water throughout the tailings, likely as a result of the dissolution of wolframite. Consistent with geochemical model calculations, results from SEM/EDS, EMP/WDS and TEM/EDS analyses indicate that secondary minerals, which occur as orange-brown coatings on grains of primary-minerals, are Fe oxyhydroxides. Examples of these secondary minerals display a fibrous habit at high resolution in the TEM. One of these minerals, which contains substantial amounts of Al, As, and Si as impurities, was identified by selected-area electron diffraction (SAED) analyses to be goethite. Another mineral contains relatively high amounts of Si, Pb, Bi, and As, and SAED analyses suggest that the mineral is two-line ferrihydrite.  相似文献   

17.
索伦石的晶体结构   总被引：1，自引：0，他引：1       下载免费PDF全文
索伦石是1961年在我国发现的一种新矿物。成分为CaO·SiO2·H2O,是人工和天然的含水硅酸钙矿物中CaO∶SiO2∶H2O=1:1:1的唯一一种矿物,因此索伦石结构的测定对了解这一类矿物的晶体化学当有助益。  相似文献   

18.
增强型地热系统(EGS)是采用人工形成地热储层的方法,从低渗透性岩体中经济地采出深层热能的人工地热系统。以CO2为载热流体的增强地热能系统(CO2-EGS)是实现CO2减排和深部地热资源开发的有效手段,系统运行时的水-岩-气相互作用对热储层孔渗特征有着重要影响,最终会影响储层的产热能力。笔者利用高温高压反应釜模拟CO2-EGS高温下的热储层-盐水-CO2的相互作用,通过对实验中反应液离子成分变化和岩样扫描电镜进行分析,结果表明:实验后的钾长石和方解石出现溶解现象,且方解石溶蚀剧烈;岩样表面出现极少量次生方解石和钠长石,并有新矿物析出,其主要组成元素为C、O、Si、Fe,为菱铁矿的中间产物。通过TOUGHREACT建立反应性溶质运移模型,模拟上述实验的化学反应过程,模拟结果和实验数据拟合较好。该研究可为CO2-EGS的水-岩-气作用机制提供地球化学数据。  相似文献   

19.
自然岩石及简单和复杂体系中实验合成或经重新平衡的尖晶石化学成分显示，在中－低压条件下，与橄榄石共存的尖晶石可含一定量的Ｓｉ，其含量随温度和压力的升高而增大。用最小二乘法对简单体系中 实验数据的热力学模拟发现，Ｓｉ在铬尖晶石中以硅酸盐尖晶石（Ｍｇ２ＳｉＯ４）形式存在，Ｍｇ２ＳｉＯ４组份在铬尖晶石中的活度ａＳＤＭＧ２ＳｉＯ４＝（ＮＳＰＭＧ／２）２＊（ＮＳＰＳｉ）２（ＮＳＰＳｉ代表以４个氧为基础的单位尖  相似文献   

20.
The template carbonization method was utilized for the production of mesoporous carbons using attapulgite as a template and sucrose as carbon precursor. Sucrose was polymerized and carbonized in the tubes of natural attapulgite using a sulfuric acid catalyst. The structure of the template and carbons were investigated by powder X-ray diffraction, transmission electron microscopy, and Nitrogen adsorption analysis techniques. At the micrometer level, the carbon material templated with the natural attapulgite had the similar morphology. Nitrogen adsorption analysis showed that the obtained porous carbons possess a wide pore size distribution and a large pore volume, especially in the range of mesopores.  相似文献   

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