电感耦合等离子体发射光谱法测定磷矿中有效五氧化二磷     

张会芳 《化工矿产地质》2016,(4):246-249

利用电感耦合等离子体发射光谱测定磷矿中的有效五氧化二磷,样品采用柠檬酸浸提处理,干过滤,滤液引入电感耦合等离子体发射光谱测定。这种方法与传统分光光度法测定有效五氧化二磷相比较,能很好的测定磷矿中有效五氧化二磷,相对标准偏差较低,结果准确。  相似文献   

High‐Precision Measurement of Molybdenum Isotopic Compositions of Selected Geochemical Reference Materials          下载免费PDF全文

Jin Li  Xiang‐kun Zhu  Suo‐han Tang  Kan Zhang 《Geostandards and Geoanalytical Research》2016,40(3):405-415

Here we describe high‐precision molybdenum isotopic composition measurements of geological reference materials, performed using multi‐collector inductively coupled plasma‐mass spectrometry (MC‐ICP‐MS). Purification of Mo for isotopic measurements was achieved by ion exchange chromatography using Bio‐Rad AG^® 1‐X8 anion exchange resin. Instrumental mass bias was corrected using ¹⁰⁰Mo‐⁹⁷Mo double spiking techniques. The precision under intermediate measurement conditions (eighteen measurement sessions over 20 months) in terms of δ^98/95Mo was 0.10‰ (2s). The measurement output was approximately four times more efficient than previous techniques, with no compromise in precision. The Mo isotopic compositions of seven geochemical reference materials, seawater (IAPSO), manganese nodules (NOD‐P‐1 and NOD‐A‐1), copper‐molybdenum ore (HV‐2), basalt (BCR‐2) and shale (SGR‐1b and SCo‐1), were measured. δ^98/95Mo values were obtained for IAPSO (2.25 ± 0.09‰), NOD‐P‐1 (?0.66 ± 0.05‰), NOD‐A‐1 (?0.48 ± 0.05‰), HV‐2 (?0.23 ± 0.10‰), BCR‐2 (0.21 ± 0.07‰), SCo‐1 (?0.24 ± 0.06‰) and SGR‐1b (0.63 ± 0.02‰) by calculating δ^98/95Mo relative to NIST SRM 3134 (0.25‰, 2s). The molybdenum isotopic compositions of IAPSO, NOD‐A‐1 and NOD‐P‐1 obtained in this study are within error of the compositions reported previously. Molybdenum isotopic compositions for BCR‐2, SCo‐1 and SGR‐1b are reported for the first time.  相似文献   

Calcium Carbonate and Phosphate Reference Materials for Monitoring Bulk and Microanalytical Determination of Sr Isotopes          下载免费PDF全文

Michael Weber  Federico Lugli  Klaus Peter Jochum  Anna Cipriani  Denis Scholz 《Geostandards and Geoanalytical Research》2018,42(1):77-89

In situ laser ablation analyses rely on the microanalytical homogeneity of reference materials (RMs) and a similar matrix and mass fraction between unknown samples and RMs to obtain reliable results. Suitable carbonate and phosphate RMs for determination of Sr isotope ratios in such materials are limited. Thus, we determined ⁸⁷Sr/⁸⁶Sr ratios of several carbonate (JCt‐1, JCp‐1, MACS‐1, MACS‐3) and phosphate (MAPS‐4, MAPS‐5, NIST SRM 1400, NIST SRM 1486) international RMs using dissolved samples and two different multi‐collector inductively coupled plasma‐mass spectrometers (MC‐ICP‐MS). Our Sr isotope data are in agreement with published data and have an improved measurement precision for some RMs. For MACS‐1, we present the first ⁸⁷Sr/⁸⁶Sr value. We tested the suitability of these materials for microanalytical analyses by LA‐MC‐ICP‐MS, with two different laser ablation systems: a conventional nanosecond laser and a state‐of‐the‐art femtosecond laser. We investigated the RMs micro‐homogeneity and compared the data with our solution data. Both laser ablation systems yielded identical ⁸⁷Sr/⁸⁶Sr ratios within uncertainty to the solution data for RMs with low interferences of REEs. Therefore, these carbonate and phosphate RMs can be used to achieve accurate and precise results for in situ Sr isotope investigations by LA‐MC‐ICP‐MS of similar materials.  相似文献   

不同温度真空热处理对FeCrMoCBY非晶合金涂层组织结构与摩擦学性能的影响研究          下载免费PDF全文

李润杰  章昕怡  康嘉杰  岳文  梁健  付志强  朱丽娜  张然 《探矿工程》2021,48(S1):61-69

深部地质钻探过程中,复杂的井下工况对钻具的钻探性能以及可靠性提出了苛刻的要求。钻具钢体表面涂覆具有耐磨耐蚀性的非晶涂层可以有效提高其服役寿命。其中Fe基非晶合金涂层因其优异的耐腐蚀抗磨损性能、较强的非晶形成能力等优势,具有重要的应用价值和较好的经济效益。本文通过大气等离子喷涂技术（Air Plasma Spray, APS）在35CrMo基体上制备得到成分为Fe₄₈Cr₁₅Mo₁₄C₁₅B₆Y₂ （at.%）的非晶合金涂层,并对其进行不同温度的真空热处理,探究了不同温度热处理对涂层基本性能和磨损失效机制的影响。结果表明：涂层经过真空热处理之后,生成的大量硬质相和成分均匀化使得涂层抗磨损性能提高;且随着热处理温度的提高,涂层磨损率逐渐减小。与未经热处理和750 ℃热处理的涂层相比,经过850 ℃热处理之后的涂层具有最佳的抗磨损性能,磨损率仅为未经热处理的Fe基非晶涂层的16.7%。热处理前后涂层的失效机制均为粘着磨损、磨粒磨损、疲劳磨损和氧化磨损。  相似文献   

Fine structure of decametric type II radio bursts     

G. P. Chernov  A. A. Stanislavsky  A. A. Konovalenko  E. P. Abranin  V. V. Dorovsky  G. O. Rucker 《Astronomy Letters》2007,33(3):192-202

We have performed a comparative analysis of the fine structure of two decametric type II bursts observed on July 17 and August 16, 2002, with the 1024-channel spectrograph of the UTR-2 radio telescope in the frequency range 18.5–29.5 MHz and with the IZMIRAN spectrograph in the frequency range 25–270 MHz. The August 16 burst was weak, ～2–5 s.f.u., but exhibited an unusual fine structure in the form of broadband fibers (Δf _e > 250–500 kHz) that drifted at a rate characteristic of type II bursts and consisted of regular narrow-band fibers (Δf _e > 50–90 kHz at 24 MHz) resembling a rope of fibers. The July 17 burst was three orders of magnitude more intense (up to 4500 s.f.u. at 20 MHz) and included a similar fiber structure. The narrow fibers were irregular and shorter in duration. They differed from an ordinary rope of fibers by the absence of absorption from the low-frequency edge and by slow frequency drift (slower than that of a type II burst). Both type II bursts were also observed in interplanetary space in the WIND/WAVES RAD2 spectra, but without any direct continuation. Analysis of the corresponding coronal mass ejections (CMEs) based on SOHO/LASCO C2 data has shown that the radio source of the type II burst detected on August 16 with UTR-2 was located between the narrow CME and the shock front trailing behind that was catching up with the CME. The July 17 type II fiber burst also occurred at the time when the shock front was catching up with the CME. Under such conditions, it would be natural to assume that the emission from large fibers is related to the passage of the shock front through narrow inhomogeneities in the CME tail. Resonant transition radiation may be the main radio emission mechanism. Both events are characterized by the possible generation of whistlers between the leading CME edge and the shock front. The whistlers excited at shock fronts manifest themselves only against the background of enhanced emission from large fibers (similar to the continuum modulation in type IV bursts). The reduction in whistler group velocity inside inhomogeneities to 760 km s^?1 may be responsible for the unusually low drift rate of the narrow fibers. The magnetic field inside inhomogeneities determined from fiber parameters at 24 MHz is ～0.9 G, while the density should be increased by at least a factor of 2.  相似文献   

基于雷电预警技术的风电设施防雷技术     

李强  王婷婷  李楠 《南京气象学院学报》2012,4(6):512-516

风力发电技术迅猛发展,单机发电量不断增加,风电机组高度已增加到上百米,风电机组叶片遭受雷击风险也随之加大.通过雷电损害实例分析风机叶片雷击灾害机理,分析雷电击中风机叶片的形成和发展过程,总结大型风机叶片的特点和风电场的环境因素,以大气电场仪的预警数据为基础,结合前沿的等离子体防雷新技术,针对风力发电机的具体情况进行改进,提出实现风电叶片主动避雷的防雷技术构想,探索一种实现风电机组设备避雷的新思路.  相似文献   

杂色鲍血淋巴双向电泳与质谱分析     

韩焘  姜敬哲  王江勇 《海洋科学》2013,37(3):102-108

以杂色鲍(Haliotisdiversicolor)血淋巴为材料进行了双向电泳研究。首先,确定了以丙酮沉淀法和RC DC 蛋白定量试剂盒为基础的蛋白制备与定量方法;其次,对样品前处理方法进行了摸索,通过500 r/min的低速离心方法分离了血细胞和血浆组分,通过35000 r/min超速离心2 h除掉了部分高丰度的血蓝蛋白,降低了高分子量区域的血蓝蛋白背景;进一步使用18 cm pH 3-10非线性胶条和标准化的电泳程序,对不同上样量的电泳银染结果进行了比较,获得了良好的双向电泳图谱;最终选取肌动蛋白、原肌球蛋白、胶原蛋白和血蓝蛋白4个蛋白点成功进行了质谱鉴定。  相似文献   

NI 493.5 nm谱线Stark加宽估算闪电放电等离子体电子密度   总被引：1，自引：1，他引：0       下载免费PDF全文

郭逸潇  袁萍  瞿海燕 《高原气象》2009,28(3):675-679

依据青海地区一次闪电回击过程的光谱,分析了NI 493.5 nm谱线的Stark加宽效应,得到加宽在1.5～2.5 nm左右,通道不同位置的谱线两边显示出稍有一些不对称性;结合NI 493.5 nm线Stark加宽的半经验参数,对通道不同位置的电子密度进行了定量计算,得到平均电子密度是1.657×1017 cm-2,并与各位置处用Hα谱线半宽得到的电子密度进行了比较,证实用NI 493.5 nm和Hα谱线半宽得到的电子密度基本一致,由NI谱线的Stark加宽估算闪电等离子体电子密度是一种实用可信的方法.数据分析表明:随着通道位置的升高,电子密度略呈减小趋势;电子密度与谱线半宽近似呈线性关系.  相似文献   

On the origin of energetic particles in the foreshock region of the Earth’s bow shock     

G. N. Kichigin 《Astronomy Letters》2009,35(4):261-269

We consider the processes related to the formation of the so-called foreshock region upstream of the Earth’s bow shock. We suggest a model based on the surfing of pick-up ions in the bow shock front in terms of which the ion acceleration mechanism in the front can be explained. We ascertain the physical conditions under which the accelerated ions lie upstream of the shock front and determine the direction of motion of the energetic ions. We conclude that it is this population of energetic ions (longitudinal beams) that plays a major role in forming the ion foreshock boundary.  相似文献   

Laboratory light-scattering measurements with Titan's aerosols analogues produced by a dusty plasma     

E. Hadamcik  J.-B. Renard  G. Cernogora  C. Szopa 《Planetary and Space Science》2009,57(13):1631-1641

The chemistry leading to the formation of solid aerosols (tholins) in Titan's atmosphere is simulated by a capacitively coupled plasma in a N₂-CH₄ gas mixture. The solid grains are produced in volume directly in the gas phase and studied ex-situ by SEM imaging and by light scattering on clouds of particles. The scattered light properties depend on the physical properties of the particles (morphologies, size distribution), as well as on the phase angle and the wavelength of the light. The particles may be aggregated or agglomerated grains. The grains size distribution is studied as a function of plasma parameters such as initial methane concentration introduced into the discharge, gas flow, absorbed RF power and plasma duration. The average grain size increases when the amount of CH₄ increases, when the gas flow decreases, and when the plasma duration increases up to a limit for each production condition.For all the samples, the absorption decreases with increasing wavelength in the visible domain. As usually found for irregular particles, the polarization phase curves have a bell-shaped positive branch and a shallow negative branch. The maximum of polarization (P_max) increases when the average grain size decreases (sub-μm-sized grains). To obtain P_max values within the range of those measured in Titan's atmosphere; the average grains diameter has to be smaller than 100 nm, in agreement with the space observations results. In the light-scattering experiment, the size of the agglomerates in the clouds is in the 40-80 μm range in equivalent diameter. As a consequence P_max increases with decreasing wavelength due to the increasing absorption, in agreement with observations of Titan from outside the atmosphere.  相似文献