陶器资源——江西红土岩开发   总被引：4，自引：0，他引：4  

王平  彭人勇  周萍华 《华东地质学院学报》2001,24(2):131-134

依据江西红土岩物质组成特征及与宜兴紫砂土的相似性，对江西红土岩进行了较系统的陶器实验与研究。江西红土岩系的化学成分、矿物成分及工艺特征适合陶器要求。按其分布规律和物质组成特征可分成两类：酸性红土岩和碱性红土岩。在详细分析两类岩系工艺性质的基础上，对江西红土岩这一陶器资源进行了产品开发。  相似文献   

黄山第四纪泥砾沉积物的成因分析   总被引：8，自引：1，他引：8  

周秉根  李刚 《冰川冻土》1992,14(4):360-365

  相似文献   

Wide-Field Camera for Gravitational Microlensing Survey: MOA-cam2     

Toshifumi Yanagisawa  Yasushi Muraki  Yutaka Matsubara  Fumio Abe  Kimiaki Masuda  Sachiyo Noda  Takahiro Sumi  Yuji Kato  Mitsuaki Fujimoto  Shuji Sato  Ian Bond  Nicholas Rattenbury  Philip Yock  Pam Kilmartin  John Hearnshaw  Micheal Reid  Denis Sullivan  Brian Carter  Richard Dodd  Garry Nankivell  Noiman Rumsey  Morihiro Honda  Maki Sekiguchi  Masanori Yoshizawa  Takashi Nakamura  Humitaka Sato  Seiji Kabe  Makoto Kobayashi  Yoshiyuki Watase  Jun Jugaku  Toshiharu Saito  Barbel Koribalsky 《Experimental Astronomy》2000,10(4):519-535

We have constructed a large, mosaic CCD camera called MOA-cam2 which has 4096 × 6144-pixelsto search for gravitational microlensing events. MOA-cam2 has three4096 × 2048-pixel SITe CCD chips, which have a very high quantum efficiency (nearly 80% in the wave region 500 to 800 nm),and three buttable sides. We have placed the threechips side by side with 100 m dead space. MOA-cam2 has been installed on the 61 cm Boller and Chivens telescope of the MOA collaboration at the Mt. John University Observatory (MJUO) in NewZealand since July 1998. The field coverage is 0.92° × 1.38° per exposure. The technical details of MOA-cam2 and the first images obtained with the Boller and Chivens telescope are presented. MOA-cam2 introduces a second phase of research on gravitational microlensing by the MOA collaboration.  相似文献   

相控误差法在少井区岩性分布研究中的应用     

唐华风  王璞珺  陈文礼  程日辉  刘万洙  张艳 《新疆地质》2006,24(4):384-388

以塔里木盆地东北地区石炭系为例进行少井波阻抗反演,以此结果研究砂泥岩发育位置、剖面形态和厚度.波阻抗资料可分辨最小厚度为20 m,比常规剖面分辨率(30 m)高,可用于沉积相分析.但是用波阻抗资料进行泥岩视厚度计算,所得结果与钻井揭示厚度相比,相对误差为 12%~-15%.经过误差分析得知,相对误差与含泥率服从单峰态分布规律,且受沉积相控制.采用相控误差法校正泥岩视厚度得到真厚度,计算结果为勘探阶段烃源岩预测提供科学依据.  相似文献   

金沙江某库区东爷庙滑坡成因分析及稳定性评价     

李宏杰  杨军  熊建平  曾祥喜  钟辉亚 《中国地质灾害与防治学报》2007,18(2):13-16

文章在对滑坡周界确定和滑坡体特征研究基础之上,从岩性条件、地质构造及地下水等方面详细分析了滑坡成因。该滑坡发生在侏罗系沙溪庙组(J2s)缓倾角红层中,地层岩性为河湖相紫红色泥质粉砂岩、泥岩和灰绿色粉砂岩互层,软硬相间,该套地层的岩性内在差异构成了滑坡产生的岩性条件。加上边坡呈顺向坡结构,顺坡向节理发育,坡角临空,岩体沿着软弱层发生滑移-拉裂破坏。通过对滑坡进行稳定性计算和分析,结果表明:该滑坡在天然状态、蓄水或地震等不利条件下,整体仍处于稳定状态,只是在相对较陡的滑坡体前缘和库水位附近地形较陡的局部部位,蓄水后可能会产生小规模失稳,但其方量不会太大,加上离坝址较远,所以不会危及工程安全。因此,通过对滑坡成因分析和稳定性评价,为工程建设和移民安置工作提供了重要的保证。  相似文献   

Early star formation and the evolution of the stellar initial mass function in galaxies     

Richard B. Larson 《Monthly notices of the Royal Astronomical Society》1998,301(2):569-581

It has frequently been suggested in the literature that the stellar IMF in galaxies was top-heavy at early times. This would be plausible physically if the IMF depended on a mass-scale such as the Jeans mass that was higher at earlier times because of the generally higher temperatures that were present then. In this paper it is suggested, on the basis of current evidence and theory, that the IMF has a universal Salpeter-like form at the upper end, but flattens below a characteristic stellar mass that may vary with time. Much of the evidence that has been attributed to a top-heavy early IMF, including the ubiquitous G-dwarf problem, the high abundance of heavy elements in clusters of galaxies, and the high rate of formation of massive stars in high-redshift galaxies, can be accounted for with such an IMF if the characteristic stellar mass was several times higher during the early stages of galaxy evolution. However, significant variations in the mass-to-light ratios of galaxies and large amounts of dark matter in stellar remnants are not as easily explained in this way, because they require more extreme and less plausible assumptions about the form and variability of the IMF. Metal-free 'population III' stars are predicted to have an IMF that consists exclusively of massive stars, and they could help to account for some of the evidence that has been attributed to a top-heavy early IMF, as well as contributing importantly to the energetics and chemical enrichment of the early Universe.  相似文献   

Dark haloes of spiral galaxies: ISO photometry     

Gerard Gilmore  & M. Unavane 《Monthly notices of the Royal Astronomical Society》1998,301(3):813-826

We exclude hydrogen-burning stars, of any mass above the hydrogen-burning limit and any metallicity, as significant contributors to the massive haloes deduced from rotation curves to dominate the outer parts of spiral galaxies. We present and analyse images of four nearly edge-on bulgeless spiral galaxies (UGC 711, NGC 2915, UGC 12426, UGC 1459) obtained with ISOCAM (The CAMera instrument on board the Infrared Space Observatory ) at 14.5 and 6.75 μm. Our sensitivity limit for detection of any diffuse infrared emission associated with the dark haloes in these galaxies is a few tens of μJy per 6 × 6 arcsec² pixel, with this limit currently set by remaining difficulties in modelling the non-linear behaviour of the detectors. All four galaxies show zero detected signal from extended non-disc emission, consistent with zero halo-like luminosity density distribution. The 95 per cent upper limit on any emission, for NGC 2915 in particular, allows us to exclude very low mass main-sequence stars ( M  > 0.08 M⊙) and young brown dwarfs (≲1 Gyr) as significant contributors to dark matter in galactic haloes. Combining our results with those of the Galactic microlensing surveys, which exclude objects with M  < 0.01 M⊙, excludes almost the entire possible mass range of compact baryonic objects from contributing to Galactic dark matter.  相似文献   

Constraining the Mass Distribution of Cluster Galaxies by Weak Lensing     

Bernhard Geiger  & Peter Schneider 《Monthly notices of the Royal Astronomical Society》1998,295(3):497-510

Analysing the weak lensing distortions of the images of faint background galaxies provides a means to constrain the average mass distribution of cluster galaxies and potentially to test the extent of their dark matter haloes as a function of the density of their environment. The observable image distortions are a consequence of the interplay between the effects of a global cluster mass distribution and the perturbations resulting from individual cluster galaxies. Starting from a reconstruction of the cluster mass distribution with conventional techniques, we apply a maximum likelihood method to infer the average properties of an ensemble of cluster galaxies. From simulations this approach is found to be reliable as long as the galaxies including their dark matter haloes only contribute a small fraction to the total mass of the system. If their haloes are extended, the galaxies contain a substantial mass fraction. In this case our method is still applicable in the outer regions of clusters, where the surface mass density is low, but yields biased estimates of the parameters describing the mass profiles of the cluster galaxies in the central part of the cluster. In that case it will be necessary to resort to more sophisticated strategies by modelling cluster galaxies and an underlying global mass distribution simultaneously. We conclude that galaxy–galaxy lensing in clusters provides a unique means to probe the presence and extent of dark haloes of cluster galaxies.  相似文献   

An excursion set model for the distribution of dark matter and dark matter haloes     

Ravi K. Sheth 《Monthly notices of the Royal Astronomical Society》1998,300(4):1057-1070

A model of the gravitationally evolved dark matter distribution, in the Eulerian space, is developed. It is a simple extension of the excursion set model that is commonly used to estimate the mass function of collapsed dark matter haloes. In addition to describing the evolution of the Eulerian space distribution of the haloes, the model allows one to describe the evolution of the dark matter itself. It can also be used to describe density profiles, on scales larger than the virial radius of these haloes, and to quantify the way in which matter flows in and out of Eulerian cells. When the initial Lagrangian space distribution is white noise Gaussian, the model suggests that the Inverse Gaussian distribution should provide a reasonably good approximation to the evolved Eulerian density field, in agreement with numerical simulations. Application of this model to clustering from more general Gaussian initial conditions is discussed at the end.  相似文献   

Mass constraints from multiphase cooling flow models     

Peter A. Thomas 《Monthly notices of the Royal Astronomical Society》1998,299(2):349-356

I review the multiphase cooling flow equations that reduce to a relatively simple form for a wide class of self-similar density distributions described by the single parameter, k , first introduced by Nulsen. It is shown that steady-state cooling flows are not consistent with all possible emissivity profiles, which can therefore be used as a test of the theory. In combination, they provide strong constraints on the temperature profile and mass distribution within the cooling radius. The model is applied to ROSAT HRI data for three rich clusters. At one extreme ( K  ∼ 1) these show evidence for cores in the mass distribution of size 110–140 h ⁻¹₅₀ kpc and have temperatures that decline towards the flow centre. At the other ( k ∈ ∞), the mass density and gas temperature both rise sharply towards the flow centre. The former are more consistent with observations which usually show a lower emission-weighted temperature within the cooling flow than from the cluster as a whole. The requirement that the solutions have a temperature gradient that is non-increasing towards the cluster centre limits the matter density gradient to be shallower than ρ_grav ∝∼  r ^−1.2 in the cluster core.  相似文献