共查询到20条相似文献，搜索用时 15 毫秒
1.
V. M. Kontorovich 《Astronomy Reports》2016,60(3):322-331
The evolution and collapse of a gaseous, self-gravitating sphere in the presence of an internal massive toroidal vortex analogous to the vortex created by the toroidal magnetic field of the Sun is considered. When thermal pressure is taken into account, for sufficiently high masses, the instability is preserved even for a polytropic index γ < 4/3. In the case of a degenerate gas, the evolution of the electrons and neutrons differs appreciably. In the ultrarelativistic limit, an interval of stablemasses arises in a neutron gas, between a minimum mass that depends on the circulation velocity in the vortex and the critical mass for the formation of a black hole. This suggests toroidal vortex fields as a possible physical origin for the observed narrow spectrum of neutron-star masses. 相似文献
2.
Individual probability-density distributions for the masses of compact objects in 20 X-ray binary systems have been constructed. The mass distributions were modeled using Monte-Carlo simulations. The closeness of the components in systems with massive optical stars was taken into account using K corrections. The parameters of the resulting black-hole mass distributions were obtained using nonparametric statistical methods. The presence of a statistically significant mass gap in the range 3–5M ⊙ is confirmed. The currently observed probability-density distributions of the compact-object masses are stable against small amounts of data contamination. 相似文献
3.
The paper analyzes the mass distribution of stellar black holes derived from the light and radial-velocity curves of optical stars in close binary systems using dynamical methods. The systematic errors inherent in this approach are discussed. These are associated primarily with uncertainties in models for the contribution from gaseous structures to the optical brightness of the systems under consideration. The mass distribution is nearly flat in the range 4–15M ⊙. This is compared with the mass distribution for black holes in massive close binaries, which can be manifest as ultrabright X-ray sources (L x >1039 erg/s) observed in other galaxies. If the X-ray luminosities of these objects correspond to the Eddington limit, the black-hole mass distribution should be described by a power law, which is incompatible with the flat shape derived dynamically from observations of close binaries in our Galaxy. One possible explanation of this discrepancy is the rapid evaporation of stellar-mass black holes predicted in recent multi-dimensional models of gravity. This hypothesis can be verified by refining the stellar black-hole mass spectrum or finding isolated or binary black holes with masses below ～3M ⊙. 相似文献
4.
Hiroshi Yamamoto Kazuaki Okamoto Yoshiyuki Kaneko Masaru Terabayashi 《Tectonophysics》2004,387(1-4):151-168
Several mafic rock masses, which have experienced eclogite facies metamorphism, are distributed in flat-lying non-eclogitic schists in an intermediate structural level (thermal core) of the Sanbagawa belt. The largest, Iratsu mass, and an associated peridotite, the Higashi-Akaishi mass, extend E–W for about 8 km, and N–S for about 3 km, and are surrounded by pelitic, basic and quartz schists. The Iratsu mass consists of metabasites of gabbroic and basaltic origin, with intercalations of ultramafic rocks, felsic gneiss, quartz schist and metacarbonate. The Iratsu mass can be divided into two layers along a WNW-trending metacarbonate layer. The Higashi-Akaishi mass consists of peridotite with intercalations of garnet clinopyroxenite. It is situated beneath the western half of the Iratsu mass, and their mutual boundary dips gently or steeply to the N or NE. These masses underwent eclogite, and subsequent epidote-amphibolite facies metamorphism as has been reported elsewhere. The Iratsu–Higashi-Akaishi masses and the surrounding rocks underwent ductile deformation under epidote-amphibolite facies (or lower P–T) metamorphic conditions. Their foliation generally trends WNW and dips moderately to the NNE, and the mineral lineation mostly plunges to the N and NE. In non-eclogitic schists surrounding the Iratsu–Higashi-Akaishi masses, the foliation generally trends WNW and dips gently or steeply to the N or S and the mineral lineation mostly plunges to the NW, N and NE. Kinematic analysis of deformation structures in outcrops and oriented samples has been performed to determine shear senses. Consistent top-to-the-north, normal fault displacements are observed in peridotite layers of the Higashi-Akaishi mass and eclogite-bearing epidote amphibolite layers of the Iratsu mass. Top-to-the-northeast or top-to-the-northwest displacements also occur in non-eclogitic pelitic–quartz schists on the northern side of the Iratsu mass. In the structural bottom of the Iratsu–Higashi-Akaishi masses and to the south, reverse fault (top-to-the-south) movements are recognized in serpentinized peridotite and non-eclogitic schists. These observations provide the following constraints on the kinematics of the rock masses: (1) northward normal displacement of Iratsu relative to Higashi-Akaishi, (2) northward normal displacement of non-eclogitic schists on the north of the Iratsu mass and (3) southward thrusting of the Iratsu–Higashi-Akaishi masses upon non-eclogitic schists in the south. The exhumation process of the Iratsu–Higashi-Akaishi masses can be explained by their southward extrusion. 相似文献
5.
开采沉陷三维损伤有限元分析 总被引：4，自引：1，他引：3
针对上覆岩体结构的复杂性,将节理、裂隙及正交各向异性岩体视为损伤岩体,建立了裂隙损伤岩体三维动态有限元分析模型,给出了较详细的三维仿真模拟有限元实施格式,完成了可考虑多种工程因素且能在WINDOWS下运行的三维模拟软件。分析模拟结果显示,对岩体结构复杂性的处理方式是可行的,所研制软件是有效的。 相似文献
6.
红旗岭矿区的南东部存在7、32、33号三个岩体,一般统称为7号岩体群。7号岩体是矿区发现含铜、镍矿最大的岩体,32与33号岩体分布在7号岩体的北西部。通过对这三个岩体的地质特征进行分析,利用3Dmine软件建模技术,对三个岩体、岩相、矿体建立三维模型。对模型进行观察、分析,结合成岩成矿地质理论,发现三个岩体是由来自7号岩体的南东部深部岩浆源生成的,岩浆由7号岩体的南东部深部向北西方向侵入,地质历史上三个岩体是一个大岩体,只是经过长期的风化剥蚀和地质构造改造形成目前的3个岩体,显示7号岩体的南东部深部具有找矿潜力。 相似文献
7.
A method for using the colors of star-forming complexes to derive the slope and upper mass limit of the initial mass function (IMF) and the age of the complex is proposed in the framework of synthetic evolutionary models of star-cluster populations. The star-formation parameters of 105 complexes in 20 spiral and irregular galaxies are determined. The IMF slopes in different star-forming complexes differ appreciably, and their dependence on the luminosities and masses of the complexes is derived. The duration of the star-formation period increases with the luminosity of the complex, and complexes with longer star-formation periods are richer in metals. The slope of the integrated IMF in a Galaxy depends on the mass spectrum of its complexes, and the upper mass limit of the IMF is lower in early-type spirals. 相似文献
8.
9.
NumericalN-body studies of the dynamical evolution of a cluster of 1000 galaxies were carried out in order to investigate the role of
dark matter in the formation of cD galaxies. Two models explicitly describing the darkmatter as a full-fledged component of
the cluster having its own physical characteristics are constructed. These treat the dark matter as a continuous underlying
substrate and as “grainy” matter. The ratio of the masses of the dark and luminous matter of the cluster is varied in the
range 3–100. The observed logarithmic spectrum dN ∼ dM / M is used as an initial mass spectrum for the galaxies. A comparative numerical analysis of the evolution of the mass spectrum,
the dynamics of mergers of the cluster galaxies, and the evolution of the growth of the central, supermassive cD galaxy suggests
that dynamical friction associated with dark matter accelerates the formation of the cD galaxy via the absorption of galaxies
colliding with it. Taking into account a dark-matter “substrate” removes the formation of multiple mass-accumulation centers,
and makes it easier to form a cD galaxy that accumulates 1–2% of the cluster mass within the Hubble time scale (3–8 billion
years), consistent with observations. 相似文献
10.
为了对松动岩体的工程特性进行系统研究,以楞古水电站厂址区边坡为例,对该边坡岩体进行了详细的地质编录和物理勘探试验,重点对节理裂隙的空间发育规律、镶嵌结构和碎裂结构岩体的发育深度及空间分布、软弱结构面发育分布规律以及边坡已有变形破坏特征这四个方面进行了系统的统计和分析,认为松动岩体是区域断裂活动和浅表生改造的结果,岩体工程效应差、变形模量低;同时结合应力测试、声波测速、高密度电磁勘探等试验成果进行分析,结果显示松动岩体具低波速（波速大部分小于3 000 m/s）、低应力（最大主应力不超过20 MPa）、强透水性（透水性系数大于10 L/（min·m·m））。认为岩体破碎主要受断层及节理裂隙影响,分析了岩体破裂松动的演化过程及特征。 相似文献
11.
裂隙岩体流固耦合问题是目前国内外研究热点之一,采用离散元软件UDEC对裂隙岩体发生节理剪胀的渗透性变化规律进行了模拟分析。基于现场调查的裂隙信息统计生成裂隙网络岩体模型。 通过固定垂直应力、不断增加应力比RS(RS=水平应力/垂直应力)使岩体出现剪胀,采用库伦滑移节理模式对岩体在剪胀过程中的渗透性变化情况进行模拟。结果发现:当应力比较小(RS3.1)时,节理水力隙宽、流速、渗透系数等参数都随着应力比的增加表现出明显的降低; 而当岩体出现剪胀现象之后(应力比大于3.1),发生剪切滑移和剪胀现象的节理控制着裂隙岩体的总体渗流行为,与不考虑节理剪胀的计算结果相比,岩体渗透能力出现了显著增长。这一结果表明,剪胀对裂隙岩体渗透性的影响是显著而不可忽视的。 相似文献
12.
The relationship between the masses and metallicities of galaxies could be non-monotonic, due to the outflow of matter in
these systems. It is shown using a simple, one-zone, chemical-dynamicalmodel that the metallicity should be a non-monotonic
function of the mass for spheroidal dwarf galaxies with low masses of M ≤ 108
M
⊙, and a monotonically growing function for galaxies with higher masses. This is consistent with observations. 相似文献
13.
红土风化壳中铁、锰质和粘土等矿物的含量高，存在大量的Ｆｅ３＋、Ｆｅ２＋、Ｍｎ２＋、Ｈ２Ｏ、（ＯＨ）１－、ＣＯ２３等离子，而这些离子团的含量决定了红土风化壳的发射波谱性状，应用ＴＭ波段对这些离子团的探测能力，就有可能识别到红土风化壳及与红土型金矿有关的地物目标。湘南地区的ＴＭ数据处理，表明了与已知红土型金矿对应的“ＫＬ特征标志色块”可作为红土型金矿成矿预测的最佳标志。 相似文献
14.
河南栾川县为全国的钼都，矿产资源丰富，已探明钼钨矿产资源与出露岩体关系密切，矿体多产在岩体或岩体接触带围岩。为进一步加强栾川矿集区的资源勘查，确定隐伏岩体的空间分布和成矿规律，对深部资源进行评价，在栾川矿集区开展了重力、磁法面积测量和CSAMT电磁法剖面测量等综合物探找矿勘查。在矿集区开展1∶2.5万重力和磁法面积测量，通过向上延拓、求导及水平梯度模等方法，提取、识别与地质相关的重磁场信息，判断隐伏岩体的分布范围，依地质模型为约束条件，对资料进行定量-半定量解释，圈出隐伏岩体的空间分布形态，构建三维地质模型，得出栾川矿集区隐伏岩体规模巨大，深部资源量丰富。依据重磁解释成果，优选隐伏岩体顶界面相对较浅的黄背岭矿区，进行CSAMT剖面测量，利用卡尼亚电阻率陡变带，对隐伏岩体的顶界面进行定位。经钻孔验证，在黄背岭矿区新发现三条钼钨矿体，矿体产在岩体顶界面上下一定范围内，在岩体的凹陷部位往往矿层厚度较大，新增钼金属量102.01万吨、WO3资源量21.66万吨。成果表明，利用钼钨矿体多产在岩体界面上下一定范围内的特征，用重力、磁法面积测量确定隐伏岩体空间分布，CSAMT剖面测量确定岩体顶界面，指导钻孔定位的物探组合方法，在栾川矿集区深部资源的勘查中成果显著，该方法组合可为“中国钼都”战略资源深部找矿提供强有力的技术支撑。 相似文献
15.
We consider models of a wormhole (i) maintained by an electromagnetic field, taking into account quantum vacuum corrections to the equation of state, (ii) maintained by a combination of the magnetic field and phantom energy, with a spherically symmetrical equation of state, and (iii) with a magnetic field and phantom matter with an anisotropic equation of state. It is shown that the quantum corrections and the density and exoticity of phantom energy or matter can be as small as is desired. For an external observer, the entrance to the tunnel appears to be a magnetic monopole of macroscopic size. The accretion of ordinary matter onto the entrance to the tunnel may result in the formation of a black hole with a radial magnetic field. We consider the possibility that some active galactic nuclei and Galactic objects may be current or former entrances to magnetic wormholes. We consider the possible existence of a broad mass spectrum for wormholes, from several billion solar masses to masses of the order of 2 kg. The Hawking effect (evaporation) does not operate in such objects due to the absence of a horizon, making it possible for them to be retained over cosmological time intervals, even if their masses are smaller than 1015 g. We also discuss a model for a binary system formed by the entrances of tunnels with magnetic fields, which could be sources of nonthermal radiation and γ-ray bursts. 相似文献
16.
We have carried out numerical simulations of the dynamical evolution of galaxy clusters taking into account merging when the relative velocities of the colliding galaxies are low. In particular, we study the evolution of the structure, mass spectrum, and velocity spectrum of a cluster of a thousand galaxies, as well as the growth of the central supermassive cD galaxy. The initial velocity dispersion of the galaxies and the rotation of the cluster were taken into account. The observed logarithmic spectrum dN ～ \(\tfrac{{dM}}{M}\) was adopted as the initial mass spectrum. The dynamical evolution of galaxy clusters, allowing for the possible merging of colliding galaxies, results in the emergence of a central supermassive galaxy, whose mass continuously increases due to mergers. This occurs only if the mass of the central galaxy becomes greater than ～0.1 of the total mass of the cluster. The observation of cD galaxies with relative masses of ～0.01 suggests that they initially formed in the cluster core, merged with nearby galaxies, and accreted intergalactic gas. The model indicates that a logarithmic galaxy mass spectrum is preserved during the cluster evolution, despite the substantial decrease in the number of galaxies in the cluster with time. The model can also reproduce the observed mass distribution with distance from the cluster center, M r ～ r 1.7. 相似文献
17.
Kim H. Esbensen Vagn F. Buchwald Dan J. Malvin John T. Wasson 《Geochimica et cosmochimica acta》1982,46(10):1913-1920
Concentrations of Re, Ir and Au are nearly constant within individual masses of the Cape York IIIAB iron meteorite, but differences between masses can be as large as a factor of 2, the extremes being Savik (5.1 μg/g Ir) and Agpalilik (2.7 μg/g Ir). The S concentration shows a still larger range from 13 mg/g in Agpalilik to 1.4 mg/g in Savik. A relatively large compositional hiatus between Dog and Agpalilik probably reflects inadequate sampling of the original material.Concentrations of Ir vary by ~10% and Au by ~3% between the ends of an 85-cm section from the Agpalilik mass of Cape York, but other sections through Agpalilik show smaller variations. These concentration ranges are much larger than expected from radial crystallization of a moderately large (radius 10 s of km) core. These variations in the Agpalilik mass may reflect dendritic crystallization, or they may have resulted from the process that produced the large concentration range among the Cape York masses.Large gradients in Re and Ir and small gradients in Ni and Au were also observed in samples within 2 cm of a large (100 cm3) troilite nodule. These gradients may reflect rapidly changing solid/liquid distribution coefficients during the final crystallization of S-rich liquid.The compositional trends among the various masses can either be explained by mixing of disparate end members followed by diffusive homogenization on a scale of m, or by dendritic crystallization on the ceiling of the IIIAB magma chamber. The mixing of a solid similar in composition to Savik with a liquid in equilibrium with this solid yields a good match to the observed trends, in which case Agpalilik consists of a mixture of 64% liquid and 36% solids. The bulk S content of the IIIAB core is calculated to be 14 mg/g on the basis of this model. 相似文献
18.
Paul R. Craddock Olivier J. Rouxel Lary A. Ball Wolfgang Bach 《Chemical Geology》2008,253(3-4):102-113
We have developed a technique for the accurate and precise determination of 34S/32S isotope ratios (δ34S) in sulfur-bearing minerals using solution and laser ablation multiple-collector inductively coupled plasma mass spectrometry (MC-ICP-MS). We have examined and determined rigorous corrections for analytical difficulties such as instrumental mass bias, unresolved isobaric interferences, blanks, and laser ablation- and matrix-induced isotopic fractionation. Use of high resolution sector-field mass spectrometry removes major isobaric interferences from O2+. Standard-sample bracketing is used to correct for the instrumental mass bias of unknown samples. Background on sulfur masses arising from memory effects and residual oxygen-tailing are typically minor (< 0.2‰, within analytical error), and are mathematically removed by on-peak zero subtraction and by bracketing of samples with standards determined at the same signal intensity (within 20%). Matrix effects are significant (up to 0.7‰) for matrix compositions relevant to many natural sulfur-bearing minerals. For solution analysis, sulfur isotope compositions are best determined using purified (matrix-clean) sulfur standards and sample solutions using the chemical purification protocol we present. For in situ analysis, where the complex matrix cannot be removed prior to analysis, appropriately matrix-matching standards and samples removes matrix artifacts and yields sulfur isotope ratios consistent with conventional techniques using matrix-clean analytes. Our method enables solid samples to be calibrated against aqueous standards; a consideration that is important when certified, isotopically-homogeneous and appropriately matrix-matched solid standards do not exist. Further, bulk and in situ analyses can be performed interchangeably in a single analytical session because the instrumental setup is identical for both. We validated the robustness of our analytical method through multiple isotope analyses of a range of reference materials and have compared these with isotope ratios determined using independent techniques. Long-term reproducibility of S isotope compositions is typically 0.20‰ and 0.45‰ (2σ) for solution and laser analysis, respectively. Our method affords the opportunity to make accurate and relatively precise S isotope measurement for a wide range of sulfur-bearing materials, and is particularly appropriate for geologic samples with complex matrix and for which high-resolution in situ analysis is critical. 相似文献
19.
This paper presents the results of a series of numerical experiments using the synthetic rock mass (SRM) approach to quantify the behaviour of jointed rock masses. Field data from a massive sulphide rock mass, at the Brunswick mine, were used to develop a discrete fracture network (DFN). The constructed DFN model was subsequently subjected to random sampling whereby 40 cubic samples, of height to width ratio of two, and of varying widths (0.05 to 10 m) were isolated. The discrete fracture samples were linked to 3D bonded particle models to generate representative SRM models for each sample size. This approach simulated the jointed rock mass as an assembly of fractures embedded into the rock matrix. The SRM samples were submitted to uniaxial loading, and the complete stress–strain behaviour of each specimen was recorded. This approach provided a way to determine the complex constitutive behaviour of large‐scale rock mass samples. This is often difficult or not possible to achieve in the laboratory. The numerical experiments suggested that higher post‐peak modulus values were obtained for smaller samples and lower values for larger sample sizes. Furthermore, the observed deviation of the recorded post‐peak modulus values decreased with sample size. The ratio of residual strength of rock mass samples per uniaxial compressive strength intact increases moderately with sample size. Consequently, for the investigated massive sulphide rock mass, the pre‐peak and post‐peak representative elemental volume size was found to be the same (7 × 7 × 14 m). Copyright © 2015 John Wiley & Sons, Ltd. 相似文献
20.
Fragments of the Chelyabinsk meteorite shower: Distribution of masses and sizes and constraints on the mass of the largest fragment 总被引：1，自引：0，他引：1
This paper reports data on the masses of fragments of the Chelyabinsk meteorite shower (fall of 15.02.2013). Assuming a lognormal distribution for the masses of fragments, the logarithm of the mean mass and standard deviation were estimated for the available data, describing the distribution density of masses and calculated diameters of fragments. Based on the dependence of the cumulative number of fragments with masses equal or greater than a given value, the mass of the largest fragment of the Chelyabinsk meteorite shower was estimated. It was shown that the most probable mass of such a fragment is hundreds of kilograms for a total mass of infalling material of 100 metric tons (t) and 1–2 t for a total mass of 1000 t, and the lower constraint for the maximum mass of the fragment is a few tens of kilograms. 相似文献