利用低强度中子源进行萤石矿中子活化测井的可行性实验研究

本文主要叙述了利用低强度中子源进行萤石矿中子活化的室内实验研究。并提及实验模型和实验技术，对实验结果进行了讨论分析，在实验的基础上，得出了应用此种方法的可行性结论。     

脉冲中子测井

属于核测井（即放射性测井）的中子测井法,目前可分成两大类:使用连续中子源的普通中子测井和使用脉冲中子源的脉冲中子测井。后者是进入六十年代以后,随着核物理技术的发展,在制成了可控的井下脉冲中子源后才开始研制试验和逐渐发展起来的一种新的测井方法。脉冲中子测井包括在井内使用脉冲中子源的各种测井法,主要有中子非弹性散射γ能谱测井、中子寿命测井和循环活化测井等。其中,能谱测井法对于划分煤层、研究煤层的组分,因而也就是解决煤质问题具有重大的意义。      

中子测井

中子测井是利用中子和物质相互作用所产生各种效应的一组测井方法。在石油测井中,它作为一种孔隙度测井法,早已普遍被应用,在国外的煤田测井中,也已成为常规方法。我国的煤田测井迄今尚未开展此项工作。为了实现测井数字化,急需增加新的测井参数,而中子法和声波法则是比较成熟的方法,特在此作一简要介绍。中子测井可分为普通中子测井和脉冲中子测井两大类。前者使用连续发射的中子源,主要解决岩层的含氢量问题,通常的中子—中子测井法及中子—伽玛测井法即属于此,是石油和煤田中常规的测井方法之一;后者使用脉冲式发射的井下中子发生器,可以指示地     

中子和密度测井找气方法的更新

中子和密度测井在复杂岩性地层中找气,如果只用中子和密度孔隙度差异性质指示气层,由于复杂岩性的干扰,容易出现多解性。本文建立的测井找气模型、刻度公式、气层下限值、指示和验证气层法则,更新了中子和密度测并找气方法,能够压制复杂岩性的干扰,排除多解性。文中给出的测井找气实例表明,采用更新后的测井找气方法指示低孔隙度复杂岩性气层,提高了中子和密度测井指示气层的分辨率、直观性和准确性,从而获得了更好的找气效果。     

基于CIFLog的铀裂变瞬发中子测井解释模块设计与研发

铀矿γ测井是一种“间接测铀”方法,铀裂变瞬发中子测井是“直接测铀”方法,中子测井技术有其独特的优势,有望替代γ测井技术。经过多年的生产应用,γ测井已经有比较成熟的数据解释软件系统,但是铀裂变瞬发中子测井没有能够投入生产的应用软件。文章根据测井软件系统CIFLog的特点和结构组成,将铀矿测井的五点式反褶积分层解释法通过模块实现,集成于CIFLog系统中,再利用CIFLog测井解释模块,对解释数据进行可视化呈现,生成专业的成果展示,为铀裂变瞬发中子测井的应用提供可靠的应用软件系统。     

碎屑岩地区低矿化度气田的气,水层识别方法—以十屋断陷八层 …

在松辽盆地十屋断陷八屋气田,由于气田水的矿化度低,使得利用电阻率曲线不能将气层与水层区分开。为了解决这个问题,作者依据中子测井的“挖掘效应”原理,提出一种识别气、水层的新方法：首先,采用声波和中子孔隙度之间的差值合成一种新的曲线－声波中子合成曲线;然后,利用自然伽马曲线等划分出砂岩储层段;最后,利用所合成的声波中子合成曲线进行判别,凡大于零者为气层,小于零则为水层。     

基于改进低秩矩阵恢复模型的测井数据去噪方法研究

在铀矿中子测井数据处理方面,受井液、地层孔隙度、岩性等因素的影响,测井的噪声数据不一定满足稀疏性的要求,传统的低秩矩阵恢复（LRMR）模型对于测井原始数据的去噪效果不佳。作者提出一种基于低秩矩阵恢复的改进模型,以提高对含复杂噪声的测井数据的去噪能力。同时把加权m1范数和加权核范数的思想引入到传统的LRMR模型中,使用F范数作为惩罚项,得到改进的LRMR模型,并应用表现效果较好的非精确增广拉格朗日乘子法（IALM）对模型进行求解。运用传统模型和改进的模型对某铀矿的中子测井数据进行去噪,并使用支持向量机、决策树算法对去噪后的数据进行矿层分类分析;实验结果表明,经过改进模型去噪处理后的测井数据分类准确度更高。改进的LRMR模型去噪能力比传统LRMR模型更强,为铀矿中子测井数据去噪提供了技术支撑。     

基于流动单元基础上的水淹层定量识别方法研究——以宝浪油田宝北区块为例

针对常规测井在低渗透油藏的水淹层解释中符合率低的问题,改变以往单纯用含油层段测井资料笼统计算含水饱和度来判断水淹层的方法,采用以流动单元为基础的新方法对水淹层进行了定量识别.首先从修正的Kozeny-Carman方程出发,将宝浪油田宝北区块的储层定量划分为5类流动单元;在此基础上将中子寿命测井结果与常规测井资料相结合,建立了不同流动单元下淡水水淹层和地层水水淹层的解释模型.用新井样点的含水饱和度数据进行了检验,运用模型计算出的含水饱和度与中子寿命测井获得的含水饱和度相比平均值只差3%.同时,对6口生产井的11个小层进行了生产测试验证,符合率达82%.     

随钻中子孔隙度测井响应特性数值模拟

随钻中子孔隙度测井在随钻地层评价中发挥重要作用, 对其响应特性研究具有重要意义.利用蒙特卡罗方法建立随钻条件下地层模型, 模拟研究随钻中子孔隙度测井响应特性.模拟结果表明: 随钻和电缆测井相同条件下中子孔隙度响应变化趋势相同, 随钻中子孔隙度曲线反映孔隙度灵敏程度高于电缆测井, 但其测井响应受钻铤影响较大; 探测深度与地层孔隙度有关, 文中条件下探测深度和纵向分辨率分别为28 cm和19 cm; 在水平井和大斜度井中, 测量方位对中子孔隙度曲线影响较大; 相对倾角α越小, 中子孔隙度曲线过渡区域中点越接近地层界面; α小于60°时, 中子孔隙度曲线受围岩影响可忽略.      

核测井曲线高分辨率处理技术及其应用

着重探讨了放射性测井曲线中自然伽马测井曲线、补偿中子测井曲线和补偿密度测井曲线的高分辨率处理方法及其应用效果。对于自然伽马及自然伽马能谱测井曲线，采用反褶积技术和有效的噪音压制技术；对于补偿中子测井曲线和补偿密度测井曲线采用了改进的α因子法。可以发现：高分辨率处理技术可明显地改善有关曲线的纵向分层能力；处理后的曲线与岩心柱状图及与微球、微电极等高分辨率曲线进行对比，其相关性有很大的改善；应用高分辨率处理后的曲线求薄层的泥质含量等参数，其相对误差明显下降。     

用于裂变径迹技术刻度的铀标准玻璃的研制

监测中子积分通量是裂变径迹技术的重要组成部分。铀玻璃监测中子积分通量是国际裂变径迹定年标准化工作组推荐的重要方法之一，铀玻璃测定法还普遍用于测定样品中的铀含量及其空间分布。本文介绍的铀标准玻璃，经过多家实验室定值测定，表明其稳定性、均匀性均达到国家一级标准物质的要求，抗酸性能达到Ⅰ级光学玻璃水平，抗潮性能达到Ⅱ级光学玻璃水平。其它性能指标均达到或超过美国国家标准局的同类产品。     

Neutron diffraction determination of the cell dimensions and thermal expansion of the fluoroperovskite KMgF3 from 293 to 3.6 K

The cell dimensions of the fluoroperovskite KMgF₃ synthesized by solid state methods have been determined by powder neutron diffraction and Rietveld refinement over the temperature range 293–3.6 K using Pt metal as an internal standard for calibration of the neutron wavelength. These data demonstrate conclusively that cubic $ Pm\overline{3} m The cell dimensions of the fluoroperovskite KMgF₃ synthesized by solid state methods have been determined by powder neutron diffraction and Rietveld refinement over the temperature range 293–3.6 K using Pt metal as an internal standard for calibration of the neutron wavelength. These data demonstrate conclusively that cubic KMgF₃ does not undergo any phase transitions to structures of lower symmetry with decreasing temperature. Cell dimensions range from 3.9924(2) ? at 293 K to 3.9800(2) ? at 3.6 K, and are essentially constant within experimental error from 50 to 3.6 K. The thermal expansion data are described using a fourth order polynomial function.     

The spin-down mechanism of the X-ray pulsar 4U 2206+54

Observations of the X-ray pulsar 4U 2206+54 obtrained over 15 years show that its period, which is now 5555 ± 9 s, is increasing dramatically. This behavior is difficult to explain using traditional scenarios for the spin evolution of compact stars. The observed spin-down rate of the neutron star in 4U 2206+54 is in good agreement with the value expected in a magnetic-accretion scenario, taking into account that, under certain conditions, the magnetic field of the accretion stream can affect the geometry and type of flow. The neutron star in this case accretes material from a dense gaseous slab with small angular momentum, which is kept in equilibrium by the magnetic field of the flow itself. A magnetic-accretion scenario can be realized in 4U 2206+54 if the magnetic-field strength at the surface of the optical counterpart to the neutron star is higher than 70 G. The magnetic field at the surface of the neutron star is 4 × 10¹² G in this scenario, in agreement with estimates based on an analysis of X-ray spectra of the pulsar.     

Elemental Concentrations in Japanese Silicate Rock Standards JA-1, JR-1 and JB-2

Data on three Japanese geochemical reference samples (JR-1, JA-1, and JB-2) are presented. Ten major and thirty-five trace element concentrations were determined using x-ray fluorescence, instrumental thermal neutron activation, thermal neutron capture prompt gamma-ray spectrometry, delayed neutron assay, automated thermal neutron activation analysis, inductively coupled plasma emission, atomic absorption, and ion selective electrode. Good agreement between the various methods and with recent literature values were obtained using error weighted mean concentrations for the samples.     

3D Simulation of Anisotropic Heat Transfer in Outer Layers of Magnetized Neutron Stars

The results of three-dimensional numerical simulation of heat transfer in the outer layers of magnetized neutron stars are presented. Determining the structure of the magnetic field on a neutron star surface is an important task of modern astrophysics. In the presence of strong magnetic fields, the medium becomes anisotropic, and the laws of heat conduction change. The tensor coefficient of thermal conductivity for magnetized degenerate plasma was obtained by Bisnovatyi-Kogan and Glushikhina by solving the Boltzmann equation with the Chapman–Enskog method. In this paper, the temperature distribution on the surface of a magnetized neutron star is obtained for magnetic fields of the dipolar and quadrupolar type, as well as for their superposition. To numerically solve the stationary temperature distribution problem in the outer layers of a magnetized neutron star, the basic (support) operator numerical method was extended to a three-dimensional case. The problem was solved on the grid which consists of tetrahedra.     

Long-period variations of pulsar emission and the dynamical ellipticity of neutron stars

Assuming that the observed periodic variations of pulsar emission are due to the free precession of the spin axis, we investigate the evolution of the rotation of a two-layer neutron star using the Hamiltonian method of Getino. We model the dynamical characteristics of a rotating neutron star using the observed variations of the emission of seven pulsars. We estimate the dependence of the period of the Chandler wobble, the period of precession of the spin axis, and the dynamical ellipticity of a neutron star on the model used to describe the super-dense neutron matter and the mass of the star.     

Evolution of close binaries and gamma-ray bursts

We analyze the late stages of evolution of massive (M ₀ ? 8 M _⊙) close binaries, from the point of view of possible mechanisms for the generation of gamma-ray bursts. It is assumed that a gamma-ray burst requires the formation of a massive (～1 M _⊙), compact (R ? 10 km) accretion disk around a Kerr black hole or neutron star. Such Kerr black holes are produced by core collapses of Wolf-Rayet stars in very close binaries, as well as by mergers of neutron stars and black holes or two neutron stars in binaries. The required accretion disks can also form around neutron stars that were formed via the collapse of ONeMg white dwarfs. We estimate the Galactic rate of events resulting in the formation of rapidly rotating relativistic objects. The computations were carried out using the “Scenario Machine.”     

Control of Cl production in carbonaceous shales by phosphate minerals

When using ³⁶Cl to date very old groundwater in regional aquifer systems, knowledge of the subsurface ³⁶Cl input into the aquifer system is essential. Although ³⁶Cl can be produced through nuclear reactions in the subsurface, in many situations, the input of ³⁶Cl into sedimentary aquifer systems by this avenue of production can be neglected. This is a valid assumption when investigating long-flowpath groundwater systems composed of sandstones, limestones, and shales of typical composition. These rock types are not sufficiently enriched in radioactive elements to produce significant ³⁶Cl in the deep subsurface. Carbonaceous shales, on the other hand, can concentrate the radioactive elements necessary to produce significant ³⁶Cl in the deep subsurface. Chlorine-36 ratios (³⁶Cl/Cl) for a suite of Late Devonian and Pennsylvanian carbonaceous shales were calculated from bulk-rock chemistry as well as measured using accelerator mass spectrometry. The poor agreement between calculated and measured ratios is the result of the assumption of chemical homogeneity used by the calculation algorithm, an assumption that was not satisfied by the carbonaceous shales. In these shales, organic matter, clay minerals, and accessory minerals are heterogeneously distributed and are physically distinct on a micron-order scale. Although organic matter and clay minerals constitute the overwhelming bulk of the shales, it is the phosphate minerals that are most important in enhancing, and suppressing, ³⁶Cl production. Minerals such as apatite and carbonate-apatite (francolite)—by including uranium, rare earth elements (REEs), and halogens—have an important impact on both neutron production and thermal neutron absorption. By incorporating both uranium and fluorine, phosphate minerals act as neutron production centers in the shale, increasing the probability of ³⁶Cl production. By incorporating REEs and chlorine, phosphate minerals also act to shield ³⁵Cl from the thermal neutron flux, effectively suppressing the production of ³⁶Cl. To reconcile the measured ³⁶Cl ratios with the ratios calculated assuming chemical homogeneity, the shales were artificially split into three fractions: organic, clay mineral, and phosphate mineral. Neutron production was calculated separately for each fraction, and the calculation results demonstrated that the phosphate fraction exerted much more control on the ³⁶Cl ratio than the organic or clay mineral fractions. By varying the uranium and chlorine contents in the phosphate fraction, a new, heterogeneous ³⁶Cl ratio was calculated that agreed with the measured ratio for the overwhelming majority of the carbonaceous shales. When using rock chemistry to calculate the ³⁶Cl ratio, rock types that show mineralogical heterogeneity on a micron scale can be divided into bulk fractions and accessory fractions for separate calculations of neutron production and neutron absorption. In this manner, a more accurate, heterogeneous ³⁶Cl ratio can be calculated for the rock as a whole.     

A new look at anomalous X-ray Pulsars

We explore the possibility of explaining Anomalous X-ray Pulsars (AXPs) and Soft Gammaray Repeaters (SGRs) in a scenario with fall-back magnetic accretion onto a young isolated neutron star. The X-ray emission of the pulsar in this case originates due to the accretion of matter onto the surface of the neutron star from a magnetic slab surrounding its magnetosphere. The spin-down rate of the neutron star expected in this picture is close to the observed value. We show that such neutron stars are relatively young and are going through the transition from the propeller state to the accretor state. The pulsar’s activity in gamma-rays is connected with its relative youth, and is enabled by energy stored in a non-equilibrium layer located in the crust of the low-mass neutron star. This energy can be released due to the mixing of matter in the neutron star crust with super heavy nuclei approaching its surface and becoming unstable. The fission of nuclei in the low-density region initiates chain reactions leading to a nuclear explosion. Outbursts are probably triggered by instability developing in the region where the matter accreted by the neutron star accumulates in the magnetic polar regions.